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73 results on '"general [Asteroids]"'

1. Morphology and spectral properties of the DART impact ejecta with VLT/MUSE

Author

C. Opitom, B. Murphy, C. Snodgrass, S. Bagnulo, S. F. Green, M. M. Knight, J. de Léon, J.-Y. Li, and D. Gardener

Subjects
Space and Planetary Science, imaging spectroscopy [Techniques], Minor planets, Astronomy and Astrophysics, Space vehicles, general [Asteroids]
Abstract

Context. On September 26, 2022, the NASA DART mission impacted the asteroid Dimorphos, the smaller component of the Didymos binary asteroid system. This provided a unique opportunity to observe, in real time, the evolution of the ejecta cloud produced by the impact and the formation of a tail. Aims. We present observations performed with the MUSE instrument at the Very Large Telescope to characterise the morphology, spectral properties, and evolution of the ejecta. The Didymos system was observed with MUSE on 11 nights from just before impact to almost one month post-impact, using both wide-field observations without adaptive optics and narrow-field observations with adaptive optics. Methods. We produced white light images that were used to study the morphology of the ejecta at different spatial scales. The spectral information was used to search for gas emission from either exposed ice or propellant, and to study the spatial and temporal variation of the ejecta dust reflectance through reflectance maps. Results. We searched for, but did not detect, emission from [OI], Xe, NH2, and H2O+ in a 1′×1′ field of view in our observations starting almost 4h after impact. We detected a number of morphological features, including a short-lived ejecta cloud visible on September 27 towards the east, spirals, clumps, and a tail that started forming only a few hours after impact. The analysis of the reflectance maps showed that the initial ejecta was bluer than the system before impact, while the tail and spirals were redder than the initial ejecta, consistent with them being made of larger particles. Over the few weeks following impact, the tail became redder. No significant colour differences could be seen between the clumps and the initial ejecta.

Published
2023

2. Energy signature of ton TNT-class impacts: analysis of the 2018 December 22 fireball over Western Pyrenees

Author

A. Malgoyre, Mar Tapia, D. Rousseu, C. Davadan, S. Jeanne, Detlef Koschny, Theresa Ott, Cyril Blanpain, D. A. Nedelcu, J. Lecubin, Pierre Vernazza, P. Cauhape, Esther Drolshagen, J. Vaubaillon, Brigitte Zanda, Agustín Sánchez-Lavega, Josep M. Trigo-Rodríguez, Mirel Birlan, J. L. Rault, S. Anghel, P. Dupouy, E. Peña-Asensio, M. Herpin, S. J. Ribas, Laurent Jorda, Jérôme Gattacceca, Ricardo Hueso, B. Tregon, Albert Rimola, François Colas, Sylvain Bouley, Ministerio de Ciencia, Innovación y Universidades (España), Diputación Foral de Bizkaia, and Eusko Jaurlaritza

Subjects
Physics, Class (set theory), Meteors, Meteoroid, photometric [Techniques], Astronomy, Astronomy and Astrophysics, Meteoroids, 010502 geochemistry & geophysics, 01 natural sciences, Asteroids: general, Meteorite, Space and Planetary Science, Asteroid, Minor plantes, 0103 physical sciences, Ton, Signature (topology), general [Asteroids], 010303 astronomy & astrophysics, Techniques: photometric, Energy (signal processing), Meteorites, 0105 earth and related environmental sciences
Abstract

Anghel, S., et al., The increase in detector sensitivity and availability in the past three decades has allowed us to derive knowledge of the meteoroid flux and impact energy into the Earth's atmosphere. We present the multi-instrument detected 2018 December 22 fireball over Western Pyrenees, and compare several techniques aiming to obtain a reliable method to be used when measuring impacts of similar scale. From trajectory data alone, we found a bulk density of 3.5 g cm-3 to be the most likely value for the Pyrenean meteoroid. This allowed to further constrain the dynamic mass, which translated into a kinetic energy of 1 ton TNT (4.184 × 109 J). For the second energy derivation, via the fireball's corrected optical radiation, we obtained a more accurate empirical relation measuring well-studied bolides. The result approximates to 1.1 ton TNT, which is notably close to the nominal dynamic result, and agrees with the lower margin of the seismic-based energy estimation, yet way lower than the infrasound estimate. Based on the relation derived in this study, we consider the nominal estimate from both the dynamic and photometric methods to be the most accurate value of deposited energy (1 ton TNT). We show that the combination of these two methods can be used to infer the meteoroid density. Among the methods presented in this paper, we found that the optical energy is the most reliable predictor of impact energy near the ton TNT-scale., S. Anghel and D. A. Nedelcu were supported by a grant of the Romanian Ministry of Research and Innovation, CCCDI - UEFISCDI, project number PN-III-P1-1.2-PCCDI-2017-0226/16PCCDI/2018, within PNCDI III. EP-A and JMT-R acknowledge funding from PGC2018-097374-B-I00 (MCI-AEI-FEDER, EU). M. Birlan work was partly supported by SEEING-IEA CNRS program. R. Hueso and A. Sánchez-Lavega were supported by Diputación Foral de Bizkaia and Gobierto Vasco IT1366-19.

Published
2021

3. Mining archival data from wide-field astronomical surveys in search of near-Earth objects

Author

Teymoor Saifollahi, Gijs Verdoes Kleijn, Rees Williams, Marco Micheli, Toni Santana-Ros, Ewout Helmich, Detlef Koschny, Luca Conversi, and Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], FOS: Physical sciences, Minor planets, Astronomy and Astrophysics, Astrometry, Space and Planetary Science, miscellaneous [Astronomical databases], observational [Methods], data analysis [Methods], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

Increasing our knowledge of the orbits and compositions of Near-Earth Objects (NEOs) is important for a better understanding of the evolution of the Solar System and of life. The detection of serendipitous NEO appearances among the millions of archived exposures from large astronomical imaging surveys can provide a contribution which is complementary to NEO surveys. Using the AstroWISE information system, this work aims to assess the detectability rate, the achieved recovery rate and the quality of astrometry when data mining the ESO archive for the OmegaCAM wide-field imager at the VST. We developed an automatic pipeline that searches for the NEO appearances inside the AstroWISE environment. Throughout the recovery process, the pipeline uses several public web-tools to identify possible images that overlap with the position of NEOs, and acquires information on the NEOs predicted position and other properties (e.g., magnitude, rate and direction of motion) at the time of observations. We have recovered 196 appearances of NEOs from a set of 968 appearances predicted to be recoverable. It includes appearances for three NEOs which were on the impact risk list at that point. These appearances were well before their discovery. The subsequent risk assessment using the extracted astrometry removes these NEOs from the risk list. We estimate a detectability rate of 0.05 per NEO at an SNR>3 for NEOs in the OmegaCAM archive. Our automatic recovery rates are 40% and 20% for NEOs on the risk list and the full list, respectively. The achieved astrometric and photometric accuracy is on average 0.12 arcsec and 0.1 mag. These results show the high potential of the archival imaging data of the ground-based wide-field surveys as useful instruments for the search, (p)recovery and characterization of NEOs. Highly automated approaches, as possible using AstroWISE, make this undertaking feasible., 13 pages, 13 figures, accepted for publication in Astronomy & Astrophysics

Published
2023

4. The determination of asteroid H and G phase function parameters using Gaia DR2

Author

W. Weidmann, M. Colazo, Rene Duffard, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), and Ministerio de Economía y Competitividad (España)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Endowment, Center of excellence, Minor planets, FOS: Physical sciences, Library science, Astronomy and Astrophysics, Surveys, Catalogues, 01 natural sciences, Asteroids: general, State agency, Space and Planetary Science, Asteroid, Observatory, 0103 physical sciences, Phase function, general [Asteroids], 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

The Gaia mission will provide the scientific community with high-quality observations of asteroids of all categories. The second release of Gaia data (DR2) was published in 2018 and consists of 22 months of observations of 14 099 known Solar system objects, mainly asteroids. The purpose of this work is to obtain a catalogue of phase function parameters (H and G) for all the asteroids that were observed during the Gaia mission and that were published in DR2. For this purpose, we introduce an algorithm capable of building this catalogue from the magnitude and UTC epoch data present in the DR2 data base. Because Gaia will never observe asteroids with a phase angle of 0° (corresponding to opposition), but with phase angles higher than 10°, we added data from ground observations (corresponding to small phase angles) and thus improved the determination of the H and G parameters of the phase function. We also built a catalogue of the parameters of the H, G1 andG2 phase function. We compared our results of the H, G functions with those of the Astorb data base and observed that the level of agreement is satisfactory. © 2021 The Author(s)., Funding from Spanish project AYA2017-89637-R is acknowledged. Financial support was received from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). MC is a doctoral fellow of CONICET (Argentina). The resources to support astorb.dat were originally provided by NASA grant NAG5-4741 (PI E. Bowell) and the Lowell Observatory endowment, and more recently by NASA PDART grant NNX16AG52G (PI N. Moskovitz).

Published
2021

5. Ground-based observability of Dimorphos DART impact ejecta: photometric predictions

Author

Fernando Moreno, Adriano Campo Bagatin, Gonzalo Tancredi, Po-Yen Liu, Bruno Domínguez, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Astronomía y Astrofísica, Moreno Fernando, Campo Bagatin Adriano, Tancredi Machado Gonzalo José, Universidad de la República (Uruguay). Facultad de Ciencias. Instituto de Física., Po-Yen Liu, Domínguez Bruno, Universidad de la República (Uruguay). Facultad de Ciencias. Instituto de Física., Ministerio de Ciencia e Innovación (España), European Commission, and Agencia Nacional de Investigación e Innovación (Uruguay)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Asteroids: general, numerical [Methods], Methods: numerical, Space and Planetary Science, general, FOS: Physical sciences, Astronomy and Astrophysics, numerical –asteroids, Astrophysics::Earth and Planetary Astrophysics, general [Asteroids], Astrophysics - Earth and Planetary Astrophysics, methods
Abstract

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The Double Asteroid Redirection Test (DART) is a NASA mission intended to crash a projectile on Dimorphos, the secondary component of the binary (65803) Didymos system, to study its orbit deflection. As a consequence of the impact, a dust cloud will be be ejected from the body, potentially forming a transient coma- or comet-like tail on the hours or days following the impact, which might be observed using ground-based instrumentation. Based on the mass and speed of the impactor, and using known scaling laws, the total mass ejected can be roughly estimated. Then, with the aim to provide approximate expected brightness levels of the coma and tail extent and morphology, we have propagated the orbits of the particles ejected by integrating their equation of motion, and have used a Monte Carlo approach to study the evolution of the coma and tail brightness. For typical power-law particle size distribution of index –3.5, with radii rrmin = 1 μm and rmax = 1 cm, and ejection speeds near 10 times the escape velocity of Dimorphos, we predict an increase of brightness of ∼3 magnitudes right after the impact, and a decay to pre-impact levels some 10 d after. That would be the case if the prevailing ejection mechanism comes from the impact-induced seismic wave. However, if most of the ejecta is released at speeds of the order of ≳100 m s−1, the observability of the event would reduce to a very short time span, of the order of 1 d or shorter. © The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society., FM acknowledges financial support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). FM also acknowledges financial support from the Spanish Plan Nacional de Astronomía y Astrofísica LEONIDAS project RTI2018-095330-B-100, and project P18-RT-1854 from Junta de Andalucía. ACB and PYL acknowledge funding by the SU-SPACE-23-SEC-2019 EC-H2020 NEO-MAPP project (GA 870377). ACB also acknowledges funding by the Spanish Ministerio de Ciencia e Innovación RTI2018-099464-B-I00 project. GT and BD acknowledge finantial support from project FCE-1-2019-1-156451 of the Agencia Nacional de Investigación e Innovación ANII (Uruguay). This work has made use of NASA’s Astrophysics Data System Bibliographic Services and of the JPL’s Horizons system.

Published
2022

6. 2001 SN263 -- the contribution of their irregular shapes on the neighborhood dynamics

Author

G Valvano, O C Winter, R Sfair, R Machado Oliveira, and G Borderes-Motta

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, Celestial mechanics, Minor planets, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, general [Asteroids], dynamical evolution and stability [Planets and satellites], Biología y Biomedicina, Astrophysics - Earth and Planetary Astrophysics, Aeronáutica
Abstract

The first proposed Brazilian mission to deep space, the ASTER mission, has the triple asteroid system (153591) 2001 SN263 as a target. One of the mission's main goals is to analyze the physical and dynamical structures of the system to understand its origin and evolution. The present work aims to analyze how the asteroid's irregular shape interferes with the stability around the system. The results show that the irregular shape of the bodies plays an important role in the dynamics nearby the system. For instance, the perturbation due to the (153591) 2001 SN263 Alpha's shape affects the stability in the (153591) 2001 SN263 Gamma's vicinity. Similarly, the (153591) 2001 SN263 Beta's irregularity causes a significant instability in its nearby environment. As expected, the prograde case is the most unstable, while the retrograde scenario presents more stability. Additionally, we investigate how the solar radiation pressure perturbs particles of different sizes orbiting the triple system. We found that particles with a 10-50 cm radius could survive the radiation pressure for the retrograde case. Meanwhile, to resist solar radiation, the particles in prograde orbit must be larger than the particles in retrograde orbits, at least one order of magnitude., Comment: 12 pages, 13 figures

Published
2022
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7. VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis

Author

J. Krajewski, P. Aurard, Philippe Lamy, Vishnu Reddy, Laurent Jorda, D. Molina, Josef Hanus, Josef Ďurech, P. Michel, F. Vachier, Nicolas Rambaux, J. Oey, Grzegorz Dudziński, P. Bartczak, A. Leroy, Michael Marsset, L. Dalmon, P. Beck, H. Le Coroller, Hiroko Hamanowa, Maëlle Neveu, Christophe Dumas, Hiromi Hamanowa, A. G. Sanchez, Zouhair Benkhaldoun, N. Payre, E. Podlewska-Gaca, Fabrice Cipriani, Raoul Behrend, Paolo Tanga, Aled Jones, Julie Castillo-Rogez, Miroslav Brož, P. Antonini, Tadeusz Michalowski, F. Livet, O. Labrevoir, J. M. Bosch, Emmanuel Jehin, Arthur Vigan, S. Fauvaud, A. Chapman, Marin Ferrais, Jérôme Berthier, Alexis Drouard, Mirel Birlan, J. Grice, R. Montaigut, J. His, L. Socha, Romain Fétick, Olivier Witasse, Pierre Vernazza, Thierry Fusco, Benoit Carry, F. Marchis, Doeon Kim, Toni Santana-Ros, Mikko Kaasalainen, Matti Viikinkoski, P. Sabin, M. Audejean, A. Marciniak, Myung-Jin Kim, Bin Yang, Agnieszka Kryszczyńska, François Colas, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Prague], Charles University [Prague] (CU), Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Tampere University of Technology [Tampere] (TUT), Search for Extraterrestrial Intelligence Institute (SETI), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of Romanian Academy, Romanian Academy, Adam Mickiewicz University in Poznań (UAM), Institut de Recherche en Horticulture et Semences (IRHS), Université d'Angers (UA)-AGROCAMPUS OUEST, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Université de Liège, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), California Institute of Technology (CALTECH), European Space Agency (ESA), TMT Observatory, The Open University [Milton Keynes] (OU), Department of Mathematics [Tampere], University of Maryland [College Park], University of Maryland System, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Hospices Civils de Lyon (HCL), Research on Healthcare Performance (RESHAPE - Inserm U1290 - UCBL1), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM), Universidad de Alicante, Universitat de Barcelona (UB), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Observatoire de Chinon, Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Observatoire de Haute-Provence (OHP), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Geneva Observatory, University of Geneva [Switzerland], Université Cadi Ayyad [Marrakech] (UCA), Héritages et Constructions dans le Texte et l'Image (HCTI), Institut Brestois des Sciences de l'Homme et de la Société (IBSHS), Université de Brest (UBO)-Université de Brest (UBO)-Université de Bretagne Sud (UBS)-Université de Brest (UBO), Observatoire du Bois de Bardon, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Laboratory for Space Research [Hong Kong] (LSR), The University of Hong Kong (HKU), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Korea Astronomy and Space Science Institute (KASI), Okayama University, Chungbuk National University, Laboratoire d'analyse et de recherche en économie et finance internationales (Larefi), Université de Bordeaux (UB), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Anunaki Observatory, Sanofi-Aventis R&D, SANOFI Recherche, Planetary Science Institute [Tucson] (PSI), Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Ministerio de Economía y Competitividad (España), Belgian Science Policy Office, National Science Foundation (US), Generalitat Valenciana, Université Côte d'Azur (UCA), Université d'Angers (UA)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-INSTITUT AGRO Agrocampus Ouest, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Agence Spatiale Européenne = European Space Agency (ESA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Université de Bretagne Sud (UBS)-Université de Brest (UBO)-Institut Brestois des Sciences de l'Homme et de la Société (IBSHS), Université de Brest (UBO), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Tampere University, and Computing Sciences

Subjects
asteroids, Rotation period, Surface (mathematics), Shell (structure), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], general [Minor planets, asteroids], Context (language use), Astrophysics, 01 natural sciences, 03 medical and health sciences, Física Aplicada, 0103 physical sciences, 111 Mathematics, observational [Methods], 010303 astronomy & astrophysics, 030304 developmental biology, Physics, Asteroids:general, 0303 health sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Minor planets, techniques: high angular resolution, Astronomy and Astrophysics, 113 Computer and information sciences, asteroids: general, Bimodality, high angular resolution [Techniques], Density distribution, 115 Astronomy and space science, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], minor planets, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], high angular resolution, Shape analysis (digital geometry)
Abstract

Vernazza, P., et al., Until recently, the 3D shape, and therefore density (when combining the volume estimate with available mass estimates), and surface topography of the vast majority of the largest (D ≥ 100 km) main-belt asteroids have remained poorly constrained. The improved capabilities of the SPHERE/ZIMPOL instrument have opened new doors into ground-based asteroid exploration. Aims. To constrain the formation and evolution of a representative sample of large asteroids, we conducted a high-angular-resolution imaging survey of 42 large main-belt asteroids with VLT/SPHERE/ZIMPOL. Our asteroid sample comprises 39 bodies with D ≥ 100 km and in particular most D ≥ 200 km main-belt asteroids (20/23). Furthermore, it nicely reflects the compositional diversity present in the main belt as the sampled bodies belong to the following taxonomic classes: A, B, C, Ch/Cgh, E/M/X, K, P/T, S, and V. Methods. The SPHERE/ZIMPOL images were first used to reconstruct the 3D shape of all targets with both the ADAM and MPCD reconstruction methods.We subsequently performed a detailed shape analysis and constrained the density of each target using available mass estimates including our own mass estimates in the case of multiple systems. Results. The analysis of the reconstructed shapes allowed us to identify two families of objects as a function of their diameters, namely spherical and elongated bodies. A difference in rotation period appears to be the main origin of this bimodality. In addition, all but one object (216 Kleopatra) are located along the Maclaurin sequence with large volatile-rich bodies being the closest to the latter. Our results further reveal that the primaries of most multiple systems possess a rotation period of shorter than 6 h and an elongated shape (c=a ≤ 0.65). Densities in our sample range from ∼1.3 g cm-3 (87 Sylvia) to ∼4.3 g cm-3 (22 Kalliope). Furthermore, the density distribution appears to be strongly bimodal with volatile-poor (P ≥ 2.7 g cm-3) and volatile-rich (P ≤ 2.2 g cm-3) bodies. Finally, our survey along with previous observations provides evidence in support of the possibility that some C-complex bodies could be intrinsically related to IDP-like P- and D-type asteroids, representing different layers of a same body (C: core; P/D: outer shell). We therefore propose that P/ D-types and some C-types may have the same origin in the primordial trans-Neptunian disk., We warmly thank the ESO staff at Paranal and in particular Henri Boffin for providing us precious support and advice throughout the entire observing programme. P.V., A.D., M.F., L.J. and B.C. were supported by CNRS/INSU/PNP. The work of T.S-R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). TRAPPIST project is funded by the Belgian Fund for Scientic Research (Fond National de la Recherche Scientique, FNRS) under the grant PDR T.0120.21. E.J. is a FNRS Senior Research Associate. F.M. is supported by the National Science Foundation under Grant No. 1743015.

Published
2021

8. Luminous efficiency based on FRIPON meteors and limitations of ablation models

Author

Björn Poppe, B. Zanda, C. A. Volpicelli, J. Vaubaillon, Jim Rowe, Detlef Koschny, Pierre Vernazza, O. Hernandez, François Colas, Dan Alin Nedelcu, M. Forcier, Sylvain Bouley, Theresa Ott, Agustín Sánchez-Lavega, Josep M. Trigo-Rodríguez, Cristina Knapic, S. Rasetti, Esther Drolshagen, Daniele Gardiol, A. Toni, M. Di Carlo, Giovanni Pratesi, H. Lamy, Giovanni B. Valsecchi, Ludovic Ferrière, Sonia Zorba, E. Peña-Asensio, Mirel Birlan, Albert Rimola, A. Malgoyre, M. Jobin, S. Jeanne, Ashley J. King, Albino Carbognani, Emmanuel Jehin, Dario Barghini, Gerhard Drolshagen, W. Riva, G. M. Stirpe, A. Grandchamps, M. Di Martino, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Meteor (satellite), 010504 meteorology & atmospheric sciences, Meteors, Context (language use), Astrophysics, 01 natural sciences, meteorites, techniques: photometric, 0103 physical sciences, meteorites, meteors, meteoroids, minor planets, asteroids: general, comets: general, techniques: photometric, atmospheric effects, methods: data analysis, Emission spectrum, meteors, data analysis [Methods], meteoroids, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Meteoroid, comets: general, photometric [Techniques], Minor planets, general [Comets], Astronomy and Astrophysics, Meteoroids, Atmospheric effects, methods: data analysis, asteroids: general, Wavelength, Meteorite, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], minor planets, Luminous efficacy, Interplanetary spaceflight, general [Asteroids], Meteorites, atmospheric effects
Abstract

Drolshagen, E., et al., [Context] In meteor physics, the luminous efficiency τ is used to convert the meteor's magnitude to the corresponding meteoroid's mass. However, a lack of sufficiently accurate verification methods or adequate laboratory tests mean that discussions around this parameter are a subject of controversy. [Aims] In this work, we aim to use meteor data obtained by the Fireball Recovery and InterPlanetary Observation to calculate the luminous efficiencies of the recorded meteors. We also show the limitations of the methods presented herein. [Methods] Deceleration-based formulas were used to calculate the masses of the pre-atmospheric meteoroids. These can in turn be compared to the meteor brightnesses to assess the luminous efficiencies of the recorded objects. Fragmentation of the meteoroids is not considered within this model. Good measurements of the meteor deceleration are required. [Results] We find τ-values, as well as the shape change coefficients, of 294 meteors and fireballs with determined masses in the range of 10-6-100 kg. The derived τ-values have a median of τmedian = 2.17%. Most of them are of the order of 0.1-10%. We present how our values are obtained, compare them with data reported in the literature, and discuss several methods. A dependence of τ on the pre-atmospheric velocity of the meteor, ve, is noticeable with a relation of τ = 0.0023 ve2.3. Furthermore, a dependence of τ on the initial meteoroid mass, Me, is found with negative linear behaviour in log-log space: τ = 0.48 Me-0.47. [Conclusions] The higher luminous efficiency of fast meteors could be explained by the higher amount of energy released. Fast meteoroids produce additional emission lines that radiate more efficiently in specific wavelengths due to the appearance of the so-called second component of higher temperature. Furthermore, the negative dependence of τ on Me implies that the radiation of smaller meteoroids is more efficient. The results of this study also show the limitations of the ablation-based model for the determination of the luminous efficiency.

Published
2021

9. Identification of asteroid groups in the z1 and z2 nonlinear secular resonances through genetic algorithms

Author

R. C. Domingos, Safwan Aljbaae, Valerio Carruba, Universidade Estadual Paulista (Unesp), and National Space Research Institute (INPE)

Subjects
010504 meteorology & atmospheric sciences, Minor (linear algebra), Data analysis, Astrophysics, Space (mathematics), 01 natural sciences, Planet, individual [Asteroids], 0103 physical sciences, Celestial mechanics, Methods, 010303 astronomy & astrophysics, Mathematical Physics, 0105 earth and related environmental sciences, Physics, Applied Mathematics, Minor planets, Astronomy and Astrophysics, Computational Mathematics, Identification (information), Nonlinear system, Space and Planetary Science, Asteroid, Modeling and Simulation, Physics::Space Physics, Precession, Astrophysics::Earth and Planetary Astrophysics, general [Asteroids]
Abstract

Made available in DSpace on 2021-06-25T11:16:16Z (GMT). No. of bitstreams: 0 Previous issue date: 2021-06-01 Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) Linear secular resonances are observed when there is a ratio between the precession period of the longitudes of pericenter or nodes of a minor body and a planet. Nonlinear secular resonances occur for higher-order combinations of frequencies. They can change the shape of asteroid families in the (a, e, sin (i)) proper elements space. Identifying asteroids in secular resonances requires performing numerical simulations, and then visually inspecting if the resonant argument is librating, which is generally a time-consuming procedure. Here, we use machine learning genetic algorithms to select the most optimal model and training set to best-fit asteroids likely to be in librating states of the z1 and z2 secular resonances. We then identify groups in domains of librating asteroids, as predicted by our algorithms, and verified whether these clusters belong to known collisional families. Using this approach, we retrieved all the asteroid families known to interact with the two resonances and identified 5 fairly robust previously unknown groups. School of Natural Sciences and Engineering São Paulo State University (UNESP) Division of Space Mechanics and Control National Space Research Institute (INPE), C.P. 515 São Paulo State University (UNESP) School of Natural Sciences and Engineering São Paulo State University (UNESP) São Paulo State University (UNESP) FAPESP: 2018/20999-6 CNPq: 30157/2017-0 CAPES: 88887.374148/2019-00

Published
2021

10. J-PLUS: A first glimpse at spectrophotometry of asteroids -- The MOOJa catalog

Author

Javier Licandro, Renato A. Dupke, Jailson S. Alcaniz, Mariano Moles, Mário De Prá, C. Hernández-Monteagudo, Jorge Márcio Carvano, Antonio Marín-Franch, Jesús A. Varela, Javier Cenarro, Carlos López-Sanjuan, Alvaro Alvarez-Candal, David Morate, Raul E. Angulo, Héctor Vázquez Ramió, Beatriz B. Siffert, A. Galarza, Laerte Sodré, A. Ederoclite, Enrique Solano-Márquez, F. M. Jiménez-Esteban, David Cristóbal-Hornillos, Max Mahlke, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), and Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil)

Subjects
Solar System, media_common.quotation_subject, Photometric system, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Photometry (optics), Astrophysics::Solar and Stellar Astrophysics, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], Minor planets, Astronomy and Astrophysics, Stars, Asteroids: general, Space and Planetary Science, Asteroid, Sky, Outlier, Astrophysics::Earth and Planetary Astrophysics, Catalogs, general [Asteroids], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. The Javalambre Photometric Local Universe Survey (J-PLUS) is an observational campaign that aims to obtain photometry in 12 ultraviolet-visible filters (0.3-1 μm) over ∼8500 deg2 of the sky observable from Javalambre (Teruel, Spain). Due to its characteristics and observation strategy, this survey will allow a great number of Solar System small bodies to be analyzed, and with improved spectrophotometric resolution with respect to previous large-area photometric surveys in optical wavelengths. Aims. The main goal of the present work is to present the first catalog of magnitudes and colors of minor bodies of the Solar System compiled using the first data release (DR1) of the J-PLUS observational campaign: the Moving Objects Observed from Javalambre (MOOJa) catalog. Methods. Using the compiled photometric data we obtained very-low-resolution reflectance (photo)spectra of the asteroids. We first used a σ-clipping algorithm in order to remove outliers and clean the data. We then devised a method to select the optimal solar colors in the J-PLUS photometric system. These solar colors were computed using two different approaches: on one hand, we used different spectra of the Sun convolved with the filter transmissions of the J-PLUS system, and on the other, we selected a group of solar-type stars in the J-PLUS DR1 according to their computed stellar parameters. Finally, we used the solar colors to obtain the reflectance spectra of the asteroids. Results. We present photometric data in the J-PLUS filters for a total of 3122 minor bodies (3666 before outlier removal), and we discuss the main issues with the data, as well as some guidelines to solve them. © ESO 2021., DM acknowledges the CNPq for the support in form of a PCI grant, and also the FAPERJ for the support in the form of a Pós-Doutorado Nota 10 grant. JMC acknowledges CPNq for support through a research fellowship. AAC acknowledges support from FAPERJ (grant E26/203.186/2016) and CNPq (grants 304971/2016-2 and 401669/2016-5), from the Universidad de Alicante under contract UATALENTO18-02, and from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) MDP ackowledges funding by the Preeminent Postdoctoral Program (P3) at the University of Central Florida. JL acknowledges support from the project AYA2015-67772-R (MINECO). AG acknowledges CAPES for the support in the form of a Phd. grant. MM acknowledges funding by the European Space Agency under the research contract C4000122918. ESM and FJE acknowledge funding by the Spanish State Research Agency (AEI) Projects AYA2017-84089 and MDM-2017-0737 at Centro de Astrobiología (CSIC-INTA), Unidad de Excelencia María de Maeztu. The present work is based on observations made with the JAST/T80 telescope for the J-PLUS project at the Observatorio Astrofísico de Javalambre in Teruel, a Spanish Infraestructura Cientifico-Técnica Singular (ICTS) owned, managed and operated by the Centro de Estudios de Física del Cosmos de Aragón (CEFCA). Data has been processed and provided by CEFCA’s Unit of Processing and Archiving Data (UPAD). Funding for the J-PLUS Project has been provided by the Governments of Spain and Aragón through the Fondo de Inversiones de Teruel; the Aragón Government through the Research Groups E96, E103, and E16_17R; the Spanish Ministry of Science, Innovation and Universities (MCIU/AEI/FEDER, UE) with grants PGC2018-097585-B-C21 and PGC2018-097585-B-C22; the Spanish Ministry of Economy and Competitiveness (MINECO) under AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, AYA2012-30789, and ICTS-2009-14; and European FEDER funding (FCDD10-4E-867, FCDD13-4E-2685). The Brazilian agencies FAPESP and the National Observatory of Brazil have also contributed to this project.

Published
2021
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11. Evidence for differentiation of the most primitive small bodies

Author

Pierre Vernazza, Tadeusz Michalowski, Bin Yang, Matti Viikinkoski, Brian Warner, Agnieszka Kryszczyńska, Alexis Drouard, Alexander Storrs, Franck Marchis, J. Grice, François Colas, Patrick Michel, Laurent Jorda, Romain Fétick, Przemyslaw Bartczak, Arthur Vigan, Josef Ďurech, Marc Neveu, Frédéric Vachier, Julie Castillo-Rogez, Emmanuel Jehin, Michael Marsset, Josef Hanus, Nicolas Rambaux, Josselin Desmars, Mikko Kaasalainen, Marin Ferrais, Jérôme Berthier, Olivier Witasse, Philippe Lamy, Zouhair Benkhaldoun, E. Podlewska-Gaca, Fabrice Cipriani, Grzegorz Dudziński, Thierry Fusco, Raoul Behrend, Christophe Dumas, Anna Marciniak, Mirel Birlan, M. Pajuelo, Paolo Tanga, Benoit Carry, T. Santana-Ros, Mark A. Wieczorek, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Maryland [College Park], University of Maryland System, NASA Goddard Space Flight Center (GSFC), Institute of Astronomy [Prague], Charles University [Prague], Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Department of Mathematics [Tampere], Tampere University of Technology [Tampere] (TUT), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Geneva Observatory, University of Geneva [Switzerland], Oukaimeden Observatory, University of Cadi Ayyad (UCA), Astronomical Institute of Romanian Academy, Romanian Academy, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Institut Polytechnique des Sciences Avancées (IPSA), Thirty Meter Telescope Observatory, The Open University [Milton Keynes] (OU), University of Tampere [Finland], HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), SETI Institute, Pontificia Universidad Católica del Perú (PUCP), Institute of Physics [Szczecin], University of Szczecin, Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Towson University [Towson, MD, United States], Center for Solar System Studies (CS3), European Southern Observatory (ESO), Czech Science Foundation, Charles University (Czech Republic), Generalitat de Catalunya, Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Charles University [Prague] (CU), Université de Genève = University of Geneva (UNIGE), Université Cadi Ayyad [Marrakech] (UCA), Agence Spatiale Européenne = European Space Agency (ESA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Tampere University, and Computing Sciences

Subjects
asteroids, Solar System, 010504 meteorology & atmospheric sciences, individual: Sylvia [Asteroids], individual: Sylvia [Minor planets, asteroids], FOS: Physical sciences, general [Minor planets, asteroids], Astrophysics, 01 natural sciences, Kuiper belt, Jupiter, Interplanetary dust cloud, Neptune, Física Aplicada, 0103 physical sciences, 111 Mathematics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Nodal precession, Sylvia, Minor planets, Astronomy and Astrophysics, general [Kuiper belt], 113 Computer and information sciences, Asteroids: general, Meteorite, 115 Astronomy and space science, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], Carbonaceous chondrite, Minor plantes, Asteroids: individual: Sylvia, Kuiper belt: general, general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

Carri, B., et al., [Context] Dynamical models of Solar System evolution have suggested that the so-called P- and D-type volatile-rich asteroids formed in the outer Solar System beyond Neptune's orbit and may be genetically related to the Jupiter Trojans, comets, and small Kuiper belt objects (KBOs). Indeed, the spectral properties of P- and D-type asteroids resemble that of anhydrous cometary dust. Aims. We aim to gain insights into the above classes of bodies by characterizing the internal structure of a large P- and D-type asteroid. [Methods] We report high-angular-resolution imaging observations of the P-type asteroid (87) Sylvia with the Very Large Telescope Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument. These images were used to reconstruct the 3D shape of Sylvia. Our images together with those obtained in the past with large ground-based telescopes were used to study the dynamics of its two satellites. We also modeled Sylvia's thermal evolution. [Results] The shape of Sylvia appears flattened and elongated (a/b 1.45; a/c 1.84). We derive a volume-equivalent diameter of 271 ± 5 km and a low density of 1378 ± 45 kg m-3. The two satellites orbit Sylvia on circular, equatorial orbits. The oblateness of Sylvia should imply a detectable nodal precession which contrasts with the fully-Keplerian dynamics of its two satellites. This reveals an inhomogeneous internal structure, suggesting that Sylvia is differentiated. [Conclusions] Sylvia's low density and differentiated interior can be explained by partial melting and mass redistribution through water percolation. The outer shell should be composed of material similar to interplanetary dust particles (IDPs) and the core should be similar to aqueously altered IDPs or carbonaceous chondrite meteorites such as the Tagish Lake meteorite. Numerical simulations of the thermal evolution of Sylvia show that for a body of such a size, partial melting was unavoidable due to the decay of long-lived radionuclides. In addition, we show that bodies as small as 130-150 km in diameter should have followed a similar thermal evolution, while smaller objects, such as comets and the KBO Arrokoth, must have remained pristine, which is in agreement with in situ observations of these bodies. NASA Lucy mission target (617) Patroclus (diameter ≈140 km) may, however, be differentiated., This work has been supported by the Czech Science Foundation through grants 20-08218S (J. Hanuš, J. Ďurech) and by the Charles University Research program No. UNCE/SCI/023. The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). This material is partially based upon work supported by the National Science Foundation under Grant No. 1743015.

Published
2021

12. Binary asteroid (31) Euphrosyne: ice-rich and nearly spherical

Author

Emmanuel Jehin, Josef Hanus, Christophe Dumas, Franck Marchis, Frédéric Vachier, Nicolas Rambaux, Pierre Vernazza, Romain Fétick, Marin Ferrais, Zouhair Benkhaldoun, M. Pajuelo, Paolo Tanga, Bin Yang, A. Marciniak, Olivier Witasse, Matti Viikinkoski, E. Podlewska-Gaca, Fabrice Cipriani, Ondrej Chrenko, Philippe Lamy, Laurent Jorda, François Colas, J. Grice, Tadeusz Michalowski, Julie Castillo-Rogez, Josef Ďurech, Mikko Kaasalainen, Grzegorz Dudziński, Michael Marsset, Patrick Michel, Mirel Birlan, Przemyslaw Bartczak, Alexis Drouard, Toni Santana-Ros, Jérôme Berthier, Miroslav Brož, Arthur Vigan, P. Ševeček, Benoit Carry, Thierry Fusco, Agnieszka Kryszczyńska, European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Institute of Astronomy [Prague], Charles University [Prague] (CU), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), University of Tampere [Finland], Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Search for Extraterrestrial Intelligence Institute (SETI), Astronomical Institute of Romanian Academy, Romanian Academy, Oukaimeden Observatory, Université Cadi Ayyad [Marrakech] (UCA), Thirty Meter Telescope Observatory, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Pontificia Universidad Católica del Perú (PUCP), Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP), Czech Science Foundation, Charles University (Czech Republic), Ministry of Education, Youth and Sports (Czech Republic), Centre National de la Recherche Scientifique (France), National Aeronautics and Space Administration (US), Generalitat Valenciana, Ministerio de Economía y Competitividad (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), and Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal

Subjects
individual: (31) Euphrosyne / minor planets [Asteroids], 010504 meteorology & atmospheric sciences, general [Minor planets, asteroids], FOS: Physical sciences, Astrophysics, Asteroids: individual: (31) Euphrosyne / minor planets, 01 natural sciences, Sphericity, law.invention, Techniques: high angular resolution, Impact crater, law, Física Aplicada, 0103 physical sciences, observational [Methods], Circular orbit, 010303 astronomy & astrophysics, individual: (31) Euphrosyne [Minor planets, asteroids], ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, high angular resolution [Techniques], Orbit, Asteroids: general, Methods: observational / minor planets, Space and Planetary Science, Asteroid, Satellite, observational / minor planets [Methods], Hydrostatic equilibrium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Astrophysics - Earth and Planetary Astrophysics, Shape analysis (digital geometry)
Abstract

Aims. Asteroid (31) Euphrosyne is one of the biggest objects in the asteroid main belt and it is also the largest member of its namesake family. The Euphrosyne family occupies a highly inclined region in the outer main belt and contains a remarkably large number of members, which is interpreted as an outcome of a disruptive cratering event. Methods. The goals of this adaptive-optics imaging study are threefold: to characterize the shape of Euphrosyne, to constrain its density, and to search for the large craters that may be associated with the family formation event. Results. We obtained disk-resolved images of Euphrosyne using SPHERE/ZIMPOL at the ESO 8.2 m VLT as part of our large program (ID: 199.C-0074, PI: Vernazza). We reconstructed its 3D shape via the ADAM shape modeling algorithm based on the SPHERE images and the available light curves of this asteroid. We analyzed the dynamics of the satellite with the Genoid meta-heuristic algorithm. Finally, we studied the shape of Euphrosyne using hydrostatic equilibrium models. Conclusions. Our SPHERE observations show that Euphrosyne has a nearly spherical shape with the sphericity index of 0.9888 and its surface lacks large impact craters. Euphrosyne's diameter is 268 ± 6 km, making it one of the top ten largest main belt asteroids. We detected a satellite of Euphrosyne - S/2019 (31) 1 - that is about 4 km across, on a circular orbit. The mass determined from the orbit of the satellite together with the volume computed from the shape model imply a density of 1665 ± 242 kg m-3, suggesting that Euphrosyne probably contains a large fraction of water ice in its interior. We find that the spherical shape of Euphrosyne is a result of the reaccumulation process following the impact, as in the case of (10) Hygiea. However, our shape analysis reveals that, contrary to Hygiea, the axis ratios of Euphrosyne significantly differ from those suggested by fluid hydrostatic equilibrium following reaccumulation., This work has been supported by the Czech Science Foundation through grant 18-09470S (J. Hanuš, O. Chrenko, P. Ševecˇek) and by the Charles University Research program No. UNCE/SCI/023. M.B. was supported by the Czech Science Foundation grant 18-04514J. Computational resources were supplied by the Ministry of Education, Youth and Sports of the Czech Republic under the projects CESNET (LM2015042) and IT4Innovations National Supercomputing Centre (LM2015070). P. Vernazza, A. Drouard, M. Ferrais and B. Carry were supported by CNRS/INSU/PNP. M.M. was supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0849 issued through the Planetary Astronomy Program. The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valen-ciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the Université de Liège, and performed in collaboration with Cadi Ayyad University of Marrakesh. E. Jehin is a FNRS Senior Research Associate.

Published
2020

13. The Zelima asteroid family: Resonant configuration and rotational fission clusters

Author

J.V. Ribeiro, Valerio Carruba, and Universidade Estadual Paulista (Unesp)

Subjects
Physics, education.field_of_study, 010504 meteorology & atmospheric sciences, Fission, Population, Minor planets, Astronomy and Astrophysics, Escape velocity, Astrophysics, Asteroid family, 01 natural sciences, Resonance (particle physics), Celestial mechanics, Secular resonance, individual: (633) Zelima [Asteroids], Space and Planetary Science, Asteroid, 0103 physical sciences, education, 010303 astronomy & astrophysics, general [Asteroids], 0105 earth and related environmental sciences
Abstract

Made available in DSpace on 2020-12-12T02:31:34Z (GMT). No. of bitstreams: 0 Previous issue date: 2020-03-01 Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP) Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) Asteroid families are groups of asteroids that are identifiable in domains of proper elements. They may be the outcome of a collision, or the product of rotational fission. Among collisional families, young asteroid families are of interest because they preserve information on the original ejection velocity field with which the asteroid fragments were expelled, and because they may host a significant population of clusters produced by rotational fission among their members. The recently identified Zelima asteroid family is unique because, apart from its very young age of less than 3 Myr, is also interacting with the z1 secular resonance, making it the third asteroid family in this peculiar configuration, after the Agnia and Padua families, and the only one for which all members are in z1 librating states. Because of its extremely young age, the orbits of its members are still very clustered in the domain (σ,dσ/dt), with σ=ϖ−ϖ6+Ω−Ω6 the resonant argument of the z1 resonance. This allow for precisely dating the family with a method not available for any other main belt group. The Zelima family, based on this argument, should be 2.5±1.5 Myr old, and conserved quantities of the z1 secular resonance show that its ejection velocity field is in a range of 1.1−0.2 +0.6 of the escape velocity from the parent body, in agreement with general results for cratering collisional families. Finally, 41.7% of the members of the Zelima family are also members of possible fission clusters, confirming the trend observed for other very young families, like the Jones and Lorre groups. São Paulo State University (UNESP) School of Natural Sciences and Engineering São Paulo State University (UNESP) School of Natural Sciences and Engineering FAPESP: 18/20999-6 CNPq: 301577/2017-0

Published
2020

14. Euclid: Identification of asteroid streaks in simulated images using StreakDet software

Author

J. Carretero, R. Kohley, Andy Taylor, Mikael Granvik, S. Kermiche, H. Israel, Cristobal Padilla, A. Secroun, Mark Cropper, Ismael Tereno, Bianca Garilli, Rafael Toledo-Moreo, Natalia Auricchio, Mauro Roncarelli, F. Pasian, G. Congedo, Richard Massey, Knud Jahnke, Frank Grupp, Massimo Brescia, E. Franceschi, M. Frailis, Felix Hormuth, D. Bonino, F. Raison, Emanuel Rossetti, R. Cledassou, Eugenio Maiorano, Ole Marggraf, Mikko Pöntinen, Luca Valenziano, René J. Laureijs, B. Kubik, Julien Zoubian, M. Fumana, Martin Kunz, Massimo Meneghetti, Bruno Altieri, V. Capobianco, P. B. Lilje, G. Polenta, C. Bodendorf, Yu Wang, Marco Castellano, Stéphane Paltani, Ivan Lloro, S. Dusini, Peter Schneider, Luca Conversi, G. Meylan, Achille A. Nucita, Santiago Serrano, Benoit Carry, Lauro Moscardini, M. Wetzstein, Thomas D. Kitching, Roberto P. Saglia, Sandrine Pires, Leonardo Corcione, G. Sirri, Pontinen, M., Granvik, M., Nucita, A. A., Conversi, L., Altieri, B., Auricchio, N., Bodendorf, C., Bonino, D., Brescia, M., Capobianco, V., Carretero, J., Carry, B., Castellano, M., Cledassou, R., Congedo, G., Corcione, L., Cropper, M., Dusini, S., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Grupp, F., Hormuth, F., Israel, H., Jahnke, K., Kermiche, S., Kitching, T., Kohley, R., Kubik, B., Kunz, M., Laureijs, R., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Massey, R., Meneghetti, M., Meylan, G., Moscardini, L., Padilla, C., Paltani, S., Pasian, F., Pires, S., Polenta, G., Raison, F., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Serrano, S., Sirri, G., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Valenziano, L., Wang, Y., Wetzstein, M., Zoubian, J., Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Particle Physics and Astrophysics, Department of Physics, Planetary-system research, Pontinen M., Granvik M., Nucita A.A., Conversi L., Altieri B., Auricchio N., Bodendorf C., Bonino D., Brescia M., Capobianco V., Carretero J., Carry B., Castellano M., Cledassou R., Congedo G., Corcione L., Cropper M., Dusini S., Frailis M., Franceschi E., Fumana M., Garilli B., Grupp F., Hormuth F., Israel H., Jahnke K., Kermiche S., Kitching T., Kohley R., Kubik B., Kunz M., Laureijs R., Lilje P.B., Lloro I., Maiorano E., Marggraf O., Massey R., Meneghetti M., Meylan G., Moscardini L., Padilla C., Paltani S., Pasian F., Pires S., Polenta G., Raison F., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Serrano S., Sirri G., Taylor A.N., Tereno I., Toledo-Moreo R., Valenziano L., Wang Y., Wetzstein M., Zoubian J., Academy of Finland, European Commission, Agenzia Spaziale Italiana, Belgian Science Policy Office, Canadian Euclid Consortium, Centre National D'Etudes Spatiales (France), Danish Space Research Institute, German Centre for Air and Space Travel, Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), Romanian Space Agency, State Secretariat for Education, Research and Innovation (Switzerland), Swiss Space Office, UK Space Agency, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Space vehicle, Streak, FOS: Physical sciences, Techniques: image processing, Astrophysics, 01 natural sciences, law.invention, Apparent magnitude, Spitzer Space Telescope, surveys, law, 0103 physical sciences, data analysis [methods], image processing [Techniques], Minor planet, Annan elektroteknik och elektronik, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Survey, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Other Electrical Engineering, Electronic Engineering, Information Engineering, numerical [Methods], Spectrometer, Pixel, Methods: numerical, 010308 nuclear & particles physics, Astronomy and Astrophysics, Photometer, 115 Astronomy, Space science, methods: data analysis, data analysi [Methods], Asteroids: general, 13. Climate action, Space and Planetary Science, Asteroid, Magnitude (astronomy), minor planets, space vehicles, OBJECTS, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Astrophysics - Earth and Planetary Astrophysics, Methods: data analysi
Abstract

[Context] The ESA Euclid space telescope could observe up to 150 000 asteroids as a side product of its primary cosmological mission. Asteroids appear as trailed sources, that is streaks, in the images. Owing to the survey area of 15 000 square degrees and the number of sources, automated methods have to be used to find them. Euclid is equipped with a visible camera, VIS (VISual imager), and a near-infrared camera, NISP (Near-Infrared Spectrometer and Photometer), with three filters., [Aims] We aim to develop a pipeline to detect fast-moving objects in Euclid images, with both high completeness and high purity., [Methods] We tested the StreakDet software to find asteroids from simulated Euclid images. We optimized the parameters of StreakDet to maximize completeness, and developed a post-processing algorithm to improve the purity of the sample of detected sources by removing false-positive detections., [Results] StreakDet finds 96.9% of the synthetic asteroid streaks with apparent magnitudes brighter than 23rd magnitude and streak lengths longer than 15 pixels (10 arcsec h-1), but this comes at the cost of finding a high number of false positives. The number of false positives can be radically reduced with multi-streak analysis, which utilizes all four dithers obtained by Euclid., [Conclusions] StreakDet is a good tool for identifying asteroids in Euclid images, but there is still room for improvement, in particular, for finding short (less than 13 pixels, corresponding to 8 arcsec h-1) and/or faint streaks (fainter than the apparent magnitude of 23)., M.P. and M.G. acknowledge funding from the Academy of Finland (projects #316292 and #299543). The Euclid Consortium acknowledges the European Space Agency and the support of a number of agencies and institutes that have supported the development of Euclid. A detailed complete list is available on the Euclid web site (http://www.euclid-ec.org). In particular, the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the Centre National d’Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency.

Published
2020

15. Physical parameters of selected Gaia mass asteroids

Author

Emmanuel Jehin, Neil Parley, E. Podlewska-Gaca, Anna Marciniak, Thomas G. Müller, Josep M. Bosch, Zouhair Benkhaldoun, Lawrence A. Molnar, L. Bernasconi, K. Sobkowiak, A. Farkas, Bojan Dintinjana, Grzegorz Dudziński, Rene Duffard, M. Audejean, Raoul Behrend, A. Chapman, K. Żukowski, Aled Jones, Erika Verebélyi, R. Poncy, Victor Ali-Lagoa, V. Asenjo, Nicolás Morales, Karolina Dziadura, J. Grice, Róbert Szakáts, R. Roy, M. Butkiewicz-Bąk, S. Geier, Bálint Seli, Przemyslaw Bartczak, D. Molina, Roman Hirsh, P. Antonini, Marin Ferrais, András Pál, Toni Santana-Ros, Herve Jacquinot, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, European Commission, National Aeronautics and Space Administration (US), Hungarian Academy of Sciences, Hungarian Scientific Research Fund, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Université de Liège, Generalitat Valenciana, and Université Cadi Ayyad

Subjects
Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, general [Minor planets, asteroids], Context (language use), Astrophysics, 7. Clean energy, 01 natural sciences, Occultation, Física Aplicada, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], Minor planets, Astronomy and Astrophysics, Radiation mechanisms: thermal, Asteroids: general, 13. Climate action, Space and Planetary Science, Asteroid, thermal [Radiation mechanisms], Physics::Space Physics, Stellar occultation, Satellite, Astrophysics::Earth and Planetary Astrophysics, Spin (aerodynamics), general [Asteroids], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Thanks to the Gaia mission, it will be possible to determine the masses of approximately hundreds of large main belt asteroids with very good precision. We currently have diameter estimates for all of them that can be used to compute their volume and hence their density. However, some of those diameters are still based on simple thermal models, which can occasionally lead to volume uncertainties as high as 20-30%. Aims. The aim of this paper is to determine the 3D shape models and compute the volumes for 13 main belt asteroids that were selected from those targets for which Gaia will provide the mass with an accuracy of better than 10%. Methods. We used the genetic Shaping Asteroids with Genetic Evolution (SAGE) algorithm to fit disk-integrated, dense photometric lightcurves and obtain detailed asteroid shape models. These models were scaled by fitting them to available stellar occultation and/or thermal infrared observations. Results. We determine the spin and shape models for 13 main belt asteroids using the SAGE algorithm. Occultation fitting enables us to confirm main shape features and the spin state, while thermophysical modeling leads to more precise diameters as well as estimates of thermal inertia values. Conclusions. We calculated the volume of our sample of main-belt asteroids for which the Gaia satellite will provide precise mass determinations. From our volumes, it will then be possible to more accurately compute the bulk density, which is a fundamental physical property needed to understand the formation and evolution processes of small Solar System bodies. © ESO 2020., The research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378 (SBNAF). Funding for the Kepler and K2 missions is provided by the NASA Science Mission directorate. L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has received funding from the LP2012-31 and LP2018-7 Lendulet grants of the Hungarian Academy of Sciences. This project has been supported by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences and by the GINOP-2.3.2-15-2016-00003 grant of the Hungarian National Research, Development and Innovation Office (NKFIH). TRAPPIST-South is a project funded by the Belgian Fonds de la Recherche Scientifique (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liege, and performed in collaboration with Cadi Ayyad University of Marrakesh. E.J. is a FNRS Senior Research Associate. "The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and operated by the Institute for Space Studies of Catalonia (IEEC)." "This article is based on observations made with the SARA telescopes (Southeastern Association for Research in Astronomy), whose node is located at the Kitt Peak National Observatory, AZ under the auspices of the National Optical Astronomy Observatory (NOAO)." "This project uses data from the SuperWASP archive. The WASP project is currently funded and operated by Warwick University and Keele University, and was originally set up by Queen's University Belfast, the Universities of Keele, St. Andrews, and Leicester, the Open University, the Isaac Newton Group, the Instituto de Astrofisica de Canarias, the South African Astronomical Observatory, and by STFC." "This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration." The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain)

Published
2020

16. Asteroid (16) Psyche’s primordial shape: A possible Jacobi ellipsoid

Author

P. Bartczak, A. Marciniak, E. Podlewska-Gaca, Bin Yang, Fabrice Cipriani, Miroslav Brož, Arthur Vigan, Tadeusz Michalowski, Julie Castillo-Rogez, F. Vachier, Patrick Michel, Benoit Carry, Olivier Witasse, François Colas, Pierre Vernazza, F. Marchis, Emmanuel Jehin, P. Lamy, Josef Hanus, Matti Viikinkoski, Nicolas Rambaux, Romain Fétick, Alexis Drouard, Toni Santana-Ros, H. Le Coroller, M. Birlan, Mikko Kaasalainen, Agnieszka Kryszczyńska, Laurent Jorda, Josef Ďurech, Michael Marsset, Grzegorz Dudziński, Paolo Tanga, Marin Ferrais, Thierry Fusco, Christophe Dumas, Jérôme Berthier, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of Charles University, Charles University [Prague] (CU), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Tampere University of Technology [Tampere] (TUT), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Adam Mickiewicz University in Poznań (UAM), European Southern Observatory (ESO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), Astronomical Observatory [Poznan], Laboratoire associé de Reconnaissance cellulaire et amélioration des plantes, Institut National de la Recherche Agronomique (INRA), Department of Mathematics [Tampere], Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Northeastern University [Shenyang], European Southern Observatory, Centre National de la Recherche Scientifique (France), Czech Science Foundation, Charles University (Czech Republic), Generalitat Valenciana, European Commission, Ministerio de Economía y Competitividad (España), Tampere University, Computing Sciences, Research group: Inverse Problems, European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Rotation period, Solar System, asteroids: individual: (16) Psyche, 010504 meteorology & atmospheric sciences, lAsteroids: individual: (16) Psyche, individual: (16) Psyche [Asteroids], Context (language use), Astrophysics, individual: (16) Psyche [lAsteroids], 01 natural sciences, law.invention, law, Física Aplicada, 0103 physical sciences, observational [Methods], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, techniques: high angular resolution, Minor planets, Astronomy and Astrophysics, Ellipsoid, asteroids: general, Psyche, high angular resolution [Techniques], 13. Climate action, Space and Planetary Science, Asteroid, 115 Astronomy and space science, minor planets, Hydrostatic equilibrium, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Shape analysis (digital geometry)
Abstract

Context. Asteroid (16) Psyche is the largest M-type asteroid in the main belt and the target of the NASA Psyche mission. It is also the only asteroid of this size (D> 200 km) known to be metal rich. Although various hypotheses have been proposed to explain the rather unique physical properties of this asteroid, a perfect understanding of its formation and bulk composition is still missing. Aims. We aim to refine the shape and bulk density of (16) Psyche and to perform a thorough analysis of its shape to better constrain possible formation scenarios and the structure of its interior. Methods. We obtained disk-resolved VLT/SPHERE/ZIMPOL images acquired within our ESO large program (ID 199.C-0074), which complement similar data obtained in 2018. Both data sets offer a complete coverage of Psyche's surface. These images were used to reconstruct the three-dimensional (3D) shape of Psyche with two independent shape modeling algorithms (MPCD and ADAM). A shape analysis was subsequently performed, including a comparison with equilibrium figures and the identification of mass deficit regions. Results. Our 3D shape along with existing mass estimates imply a density of 4.20 ± 0.60 g cm-3, which is so far the highest for a solar system object following the four telluric planets. Furthermore, the shape of Psyche presents small deviations from an ellipsoid, that is, prominently three large depressions along its equator. The flatness and density of Psyche are compatible with a formation at hydrostatic equilibrium as a Jacobi ellipsoid with a shorter rotation period of ∼3h. Later impacts may have slowed down Psyche's rotation, which is currently ∼4.2 h, while also creating the imaged depressions. Conclusions. Our results open the possibility that Psyche acquired its primordial shape either after a giant impact while its interior was already frozen or while its interior was still molten owing to the decay of the short-lived radionuclide 26Al., Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.C-0074 (principal investigator: P. Vernazza). P. Vernazza, A. Drouard, M. Ferrais and B. Carry were supported by CNRS/INSU/PNP. J.H. and J.D. were supported by grant 18-09470S of the Czech Science Foundation and by the Charles University Research Programme no. UNCE/SCI/023. E.J. is F.R.S.-FNRS Senior Research Associate. The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE).

Published
2020

17. Periodic orbits of the retrograde coorbital problem

Author

M. H. M. Morais, Fathi Namouni, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidade Estadual Paulista (Unesp), and CS 24229

Subjects
Solar System, FOS: Physical sciences, Dynamical Systems (math.DS), Celestial mechanics - minor planets, 01 natural sciences, Resonance (particle physics), Jupiter, 0103 physical sciences, FOS: Mathematics, Mathematics - Dynamical Systems, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Retrograde motion, Astronomy and Astrophysics, General [Asteroids], Nonlinear Sciences - Chaotic Dynamics, Celestial mechanics, Mean motion, Classical mechanics, Space and Planetary Science, Asteroid, Orbit (dynamics), Astrophysics::Earth and Planetary Astrophysics, Chaotic Dynamics (nlin.CD), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

Asteroid (514107) Kaepaokaawela is the first example of an object in the 1/1 mean motion resonance with Jupiter with retrograde motion around the Sun. Its orbit was shown to be stable over the age of the Solar System which implies that it must have been captured from another star when the Sun was still in its birth cluster. Kaepaokaawela orbit is also located at the peak of the capture probability in the coorbital resonance. Identifying the periodic orbits that Kaepaokaawela and similar asteroids followed during their evolution is an important step towards precisely understanding their capture mechanism. Here, we find the families of periodic orbits in the two-dimensional retrograde coorbital problem and analyze their stability and bifurcations into three-dimensional periodic orbits. Our results explain the radical differences observed in 2D and 3D coorbital capture simulations. In particular, we find that analytical and numerical results obtained for planar motion are not always valid at infinitesimal deviations from the plane., Comment: 7 pages, to appear in Monthly Notices of the Royal Astronomical Society

Published
2019

18. Luminous efficiency of meteors derived from ablation model after assessment of its range of validity

Author

M. Di Carlo, Ashley J. King, Esther Drolshagen, Mirel Birlan, Pierre Vernazza, M. Forcier, Ludovic Ferrière, E. Peña-Asensio, Theresa Ott, Dan Alin Nedelcu, C. A. Volpicelli, François Colas, O. Hernandez, Sylvain Bouley, Daniele Gardiol, Cristina Knapic, Giovanni Pratesi, Agustín Sánchez-Lavega, Josep M. Trigo-Rodríguez, H. Lamy, G. M. Stirpe, S. Rasetti, Giovanni B. Valsecchi, Jim Rowe, Sonia Zorba, Albert Rimola, J. Vaubaillon, Brigitte Zanda, S. Jeanne, A. Toni, M. Di Martino, M. Jobin, Albino Carbognani, Björn Poppe, Gerhard Drolshagen, A. Grandchamps, Emmanuel Jehin, W. Riva, Detlef Koschny, Dario Barghini, A. Malgoyre, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Meteors, 010504 meteorology & atmospheric sciences, Context (language use), Astrophysics, 01 natural sciences, meteorites, techniques: photometric, 0103 physical sciences, Range (statistics), meteorites, meteors, meteoroids, minor planets, asteroids: general, comets: general, techniques: photometric, atmospheric effects, methods: data analysis, meteors, data analysis [Methods], meteoroids, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Meteoroid, comets: general, photometric [Techniques], Relative velocity, Minor planets, general [Comets], Astronomy and Astrophysics, Meteoroids, Function (mathematics), Atmospheric effects, methods: data analysis, asteroids: general, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Asteroid, minor planets, Meteorities, Luminous efficacy, Interplanetary spaceflight, general [Asteroids], atmospheric effects
Abstract

Drolshagen, E., et al., [Context] The luminous efficiency, τ, can be used to compute the pre-Atmospheric masses of meteoroids from corresponding recorded meteor brightnesses. The derivation of the luminous efficiency is non-Trivial and is subject to biases and model assumptions. This has led to greatly varying results in the last decades of studies. [Aims] The present paper aims to investigate how a reduction in various observational biases can be achieved to derive (more) reliable values for the luminous efficiency. [Methods] A total of 281 meteors observed by the Fireball Recovery and InterPlanetary Observation Network (FRIPON) are studied. The luminous efficiencies of the events are computed using an ablation-based model. The relations of τ as a function of the pre-Atmospheric meteoroid velocity, ve, and mass, Me, are studied. Various aspects that could render the method less valid, cause inaccuracies, or bias the results are investigated. On this basis, the best suitable meteors were selected for luminous efficiency computations. [Results] The presented analysis shows the limits of the used method. The most influential characteristics that are necessary for reliable results for the τ computation were identified. We study the dependence of τ on the assumed meteoroid's density, ρ, and include improved ρ-values for objects with identified meteoroid stream association. Based on the discovered individual biases and constraints we create a pre-debiased subset of 54 well-recorded events with a relative velocity change >80%, a final height

Published
2021

19. The disturbing function for polar Centaurs and transneptunian objects

Author

Fathi Namouni, M. H. M. Morais, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CS 34229, and Universidade Estadual Paulista (Unesp)

Subjects
Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, 01 natural sciences, Planet, Celestial mechanics, 0103 physical sciences, Trans-Neptunian object, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Minor planets, Oort Cloud, Resonance, Astronomy and Astrophysics, Classical mechanics, Amplitude, Space and Planetary Science, Polar, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Series expansion, general [Asteroids], general -Kuiper belt: general [Comets], Astrophysics - Earth and Planetary Astrophysics
Abstract

The classical disturbing function of the three-body problem is based on an expansion of the gravitational interaction in the vicinity of nearly coplanar orbits. Consequently, it is not suitable for the identification and study of resonances of the Centaurs and transneptunian objects on nearly polar orbits with the solar system planets. Here, we provide a series expansion algorithm of the gravitational interaction in the vicinity of polar orbits and produce explicitly the disturbing function to fourth order in eccentricity and inclination cosine. The properties of the polar series differ significantly from those of the classical disturbing function: the polar series can model any resonance as the expansion order is not related to the resonance order. The powers of eccentricity and inclination of the force amplitude of a $p$:$q$ resonance do not depend on the value of the resonance order $|p-q|$ but only on its parity. Thus all even resonance order eccentricity amplitudes are $\propto e^2$ and odd ones $\propto e$ to lowest order in eccentricity $e$. With the new findings on the structure of the polar disturbing function and the possible resonant critical arguments, we illustrate the dynamics of the polar resonances 1:3, 3:1, 2:9 and 7:9 where transneptunian object 471325 could currently be locked., 18 pages, 9 figures, 7 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2017

20. Explaining the variability of WD 1145+017 with simulations of asteroid tidal disruption

Author

Dimitri Veras, Philip J. Carter, Zoë M. Leinhardt, and Boris T. Gaensicke

Subjects
dynamical evolution and stability [planets and satellites], media_common.quotation_subject, FOS: Physical sciences, Astrophysics, 01 natural sciences, Mantle (geology), rings [planets and satellites], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), Eccentricity (behavior), white dwarfs [stars], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Astronomy, White dwarf, numerical [methods], Astronomy and Astrophysics, Debris, general [asteroids], Planetary science, physical evolution [planets and satellites], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Asteroid, Roche limit, minor planets, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Post-main-sequence planetary science has been galvanised by the striking variability, depth and shape of the photometric transit curves due to objects orbiting white dwarf WD 1145+017, a star which also hosts a dusty debris disc and circumstellar gas, and displays strong metal atmospheric pollution. However, the physical properties of the likely asteroid which is discharging disintegrating fragments remain largely unconstrained from the observations. This process has not yet been modelled numerically. Here, we use the N-body code PKDGRAV to compute dissipation properties for asteroids of different spins, densities, masses, and eccentricities. We simulate both homogeneous and differentiated asteroids, for up to two years, and find that the disruption timescale is strongly dependent on density and eccentricity, but weakly dependent on mass and spin. We find that primarily rocky differentiated bodies with moderate (~3-4 g/cm^3) bulk densities on near-circular (e, Comment: Accepted in MNRAS. Movies here!: http://www.star.bris.ac.uk/pcarter/WD1145_asteroid_disruption/

Published
2016

21. Identification of asteroids using the Virtual Observatory: the WFCAM Transit Survey

Author

M. Mahlke, M. Cortés-Contreras, S. Barceló Forteza, Enrique Solano, Josef Ďurech, Benoit Carry, F. M. Jiménez-Esteban, A. Velasco, Carlos Rodrigo, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Contreras, M. [0000-0003-3734-9866], Rodrigo Blanco, C. [0000-0001-6068-0077], Jiménez Esteban, F. M. [0000-0002-6985-9476], Carry, B. [0000-0001-5242-3089], Solano, E. [0000-0003-1885-5130], Agencia Estatal de Investigación (AEI), European Space Agency (ESA), Instituto Nacional de Técnica Aeroespacial (INTA), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Tec2Space-CM project, Grant Agency of the Czech Republic, Unidad de Excelencia Científica María de Maeztu del Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, and Ministerio de Economía y Competitividad (MINECO)

Subjects
010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Virtual observatory, Astronomical survey, 01 natural sciences, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Virtual observatory tools, Ecliptic, Astronomy, Minor planets, Astronomy and Astrophysics, Exoplanet, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Asteroid, Sky, general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

The nature and physical properties of asteroids, in particular those orbiting in the near-Earth space, are of scientific interest and practical importance. Exoplanet surveys can be excellent resources to detect asteroids, both already known and new objects. This is due to their similar observing requirements: large fields of view, long sequences, and short cadence. If the targeted fields are not located far from the ecliptic, many asteroids will cross the field of view occasionally. We present two complementary methodologies to identify asteroids serendipitously observed in large-area astronomical surveys. One methodology focuses on detecting already known asteroids using the Virtual Observatory tool SkyBoT, which predicts their positions and motions in the sky at a specific epoch. The other methodology applies the ssos pipeline, which is able to identify known and new asteroids based on their apparent motion. The application of these methods to the 6.4 deg2 of the sky covered by the Wide-Field CAMera Transit Survey in the J-band is described. We identified 15 661 positions of 1821 different asteroids. Of them, 182 are potential new discoveries. A publicly accessible online, Virtual Observatory compliant catalogue was created. We obtained the shapes and periods for five of our asteroids from their light curves built with additional photometry taken from external archives. We demonstrated that our methodologies are robust and reliable approaches to find, at zero cost of observing time, asteroids observed by chance in astronomical surveys. Our future goal is to apply them to other surveys with adequate temporal coverage. This research has been financed by ASTERICS, a project supported by the European Commission Framework Programme Horizon 2020 Research and Innovation action under grant agreement no. 653477. This research has made use of the Spanish Virtual Observatory (http://svo.cab.inta-csic.es) supported from the Spanish MINECO/FEDER through grant no. AYA2017-84089-P. MCC and FJE acknowledge financial support from the Tec2Space-CM project (P2018/NMT-4291). SBF acknowledge support by the Spanish State Research Agency (AEI) through project no. ESP2017-87676C5-1-R and no. MDM-2017-0737 Unidad de Excelencia 'Maria de Maeztu'-Centro de Astrobiolog'ia (CSIC-INTA). This research has made use of Topcat (Taylor 2005) and STILTS (Taylor 2006). This research has made use of 'Aladin sky atlas' developed at CDS, Strasbourg Observatory, France. This research has made use of IMCCE's SkyBoT VO tool (Berthier et al. 2006). The work of J. D was supported by the grant 18-04514J of the Czech Science Foundation. MM is funded by the European Space Agency under the research contract C4000122918; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737). Peer review

Published
2019

22. The critical binary star separation for a planetary system origin of white dwarf pollution

Author

Dimitri Veras, Siyi Xu, Alberto Rebassa-Mansergas, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
X-ray binary, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, outflows, Black dwarf, general [binaries], Intermediate polar, Planet, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, winds [stars], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics::Atmospheric and Oceanic Physics, Astrophysics::Galaxy Astrophysics, QB, Physics, atmospheres [stars], Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy, White dwarf, White dwarfs, Astronomy and Astrophysics, Planetary system, Estels nans, general [asteroids], abundances [stars], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], minor planets, Astrophysics::Earth and Planetary Astrophysics, Blue dwarf, Astrophysics - Earth and Planetary Astrophysics
Abstract

The atmospheres of between one quarter and one half of observed single white dwarfs in the Milky Way contain heavy element pollution from planetary debris. The pollution observed in white dwarfs in binary star systems is, however, less clear, because companion star winds can generate a stream of matter which is accreted by the white dwarf. Here we (i) discuss the necessity or lack thereof of a major planet in order to pollute a white dwarf with orbiting minor planets in both single and binary systems, and (ii) determine the critical binary separation beyond which the accretion source is from a planetary system. We hence obtain user-friendly functions relating this distance to the masses and radii of both stars, the companion wind, and the accretion rate onto the white dwarf, for a wide variety of published accretion prescriptions. We find that for the majority of white dwarfs in known binaries, if pollution is detected, then that pollution should originate from planetary material., Comment: Accepted for publication in MNRAS

Published
2018

23. The TROY project: II. Multi-technique constraints on exotrojans in nine planetary systems

Author

Monika Lendl, Philippe Robutel, M. Mallonn, A. Leleu, J. J. Neal, Alexandre C. M. Correia, Jorge Lillo-Box, Henri M. J. Boffin, João P. Faria, Pedro Figueira, Nuno C. Santos, David Barrado, Hannu Parviainen, European Southern Observatory (ESO), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Departamento de Fisica [Aveiro], Universidade de Aveiro, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Universidade do Porto = University of Porto, and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
fundamental parameters [Planets and satellites], Lagrangian point, FOS: Physical sciences, Context (language use), Astrophysics, transits [Techniques], 01 natural sciences, techniques: photometric, Planet, 0103 physical sciences, techniques: radial velocities, radial velocity [Techniques], planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Minor planets, Astronomy and Astrophysics, Planetary system, Exoplanet, asteroids: general, planets and satellites: gaseous planets, Radial velocity, gaseous planets [Planets and satellites], Space and Planetary Science, Asteroid, Trojan, minor planets, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

Co-orbital bodies are the byproduct of planet formation and evolution, as we know from the Solar System. Although planet-size co-orbitals do not exists in our planetary system, dynamical studies show that they can remain stable for long periods of time in the gravitational well of massive planets. Should they exist, their detection is feasible with the current instrumentation. In this paper, we present new ground-based observations searching for these bodies co-orbiting with nine close-in (P, Accepted for publication in A&A, 18 pages, 13 figures, 12 tables. TROY project website: http://www.sc.eso.org/~jlillobo/troy/

Published
2018
Full Text
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24. Gaia Data Release 2. Summary of the contents and survey properties

Author

Collaboration, G., Brown, A., Vallenari, A., Prusti, T., de Bruijne, J., Babusiaux, C., Bailer-Jones, C., Biermann, M., Evans, D., Eyer, L., Jansen, F., Jordi, C., Klioner, S., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H., Soubiran, C., van Leeuwen, F., Walton, N., Arenou, F., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Lattanzi, M., Bakker, J., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., De Angeli, F., Fabricius, C., Guerra, R., Holl, B., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Panuzzo, P., Portell, J., Riello, M., Seabroke, G., Tanga, P., Thévenin, F., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Teyssier, D., Altmann, M., Andrae, R., Audard, M., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Burgess, P., Busso, G., Carry, B., Cellino, A., Clementini, G., Clotet, M., Creevey, O., Davidson, M., De Ridder, J., Delchambre, L., Dell'Oro, A., Ducourant, C., Fernández-Hernández, J., Fouesneau, M., Frémat, Y., Galluccio, L., García-Torres, M., González-Núñez, J., González-Vidal, J., Gosset, E., Guy, L., Halbwachs, J., Hambly, N., Harrison, D., Hernández, J., Hestroffer, D., Hodgkin, S., Hutton, A., Jasniewicz, G., Jean-Antoine-Piccolo, A., Jordan, S., Korn, A., Krone-Martins, A., Lanzafame, A., Lebzelter, T., Löffler, W., Manteiga, M., Marrese, P., Martín-Fleitas, J., Moitinho, A., Mora, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J., Recio-Blanco, A., Richards, P., Rimoldini, L., Robin, A., Sarro, L., Siopis, C., Smith, M., Sozzetti, A., Süveges, M., Torra, J., van Reeven, W., Abbas, U., Abreu Aramburu, A., Accart, S., Aerts, C., Altavilla, G., Álvarez, M., Alvarez, R., Alves, J., Anderson, R., Andrei, A., Anglada Varela, E., Antiche, E., Antoja, T., Arcay, B., Astraatmadja, T., Bach, N., Baker, S., Balaguer-Núñez, L., Balm, P., Barache, C., Barata, C., Barbato, D., Barblan, F., Barklem, P., Barrado, D., Barros, M., Barstow, M., Bartholomé Muñoz, S., Bassilana, J., Becciani, U., Bellazzini, M., Berihuete, A., Bertone, S., Bianchi, L., Bienaymé, O., Blanco-Cuaresma, S., Boch, T., Boeche, C., Bombrun, A., Borrachero, R., Bossini, D., Bouquillon, S., Bourda, G., Bragaglia, A., Bramante, L., Breddels, M., Bressan, A., Brouillet, N., Brüsemeister, T., Brugaletta, E., Bucciarelli, B., Burlacu, A., Busonero, D., Butkevich, A., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzaro, G., Cantat-Gaudin, T., Carballo, R., Carlucci, T., Carrasco, J., Casamiquela, L., Castellani, M., Castro-Ginard, A., Charlot, P., Chemin, L., Chiavassa, A., Cocozza, G., Costigan, G., Cowell, S., Crifo, F., Crosta, M., Crowley, C., Cuypers, J., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., de Laverny, P., De Luise, F., De March, R., de Martino, D., de Souza, R., de Torres, A., Debosscher, J., del Pozo, E., Delbo, M., Delgado, A., Delgado, H., Di Matteo, P., Diakite, S., Diener, C., Distefano, E., Dolding, C., Drazinos, P., Durán, J., Edvardsson, B., Enke, H., Eriksson, K., Esquej, P., Eynard Bontemps, G., Fabre, C., Fabrizio, M., Faigler, S., Falcão, A., Farràs Casas, M., Federici, L., Fedorets, G., Fernique, P., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fraile, E., Fraser, M., Frézouls, B., Gai, M., Galleti, S., Garabato, D., García-Sedano, F., Garofalo, A., Garralda, N., Gavel, A., Gavras, P., Gerssen, J., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Glass, F., Gomes, M., Granvik, M., Gueguen, A., Guerrier, A., Guiraud, J., Gutiérrez-Sánchez, R., Haigron, R., Hatzidimitriou, D., Hauser, M., Haywood, M., Heiter, U., Helmi, A., Heu, J., Hilger, T., Hobbs, D., Hofmann, W., Holland, G., Huckle, H., Hypki, A., Icardi, V., Janßen, K., Jevardat de Fombelle, G., Jonker, P., Juhász, Á., Julbe, F., Karampelas, A., Kewley, A., Klar, J., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, M., Kontizas, E., Koposov, S., Kordopatis, G., Kostrzewa-Rutkowska, Z., Koubsky, P., Lambert, S., Lanza, A., Lasne, Y., Lavigne, J., Le Fustec, Y., Le Poncin-Lafitte, C., Lebreton, Y., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H., Lister, T., Livanou, E., Lobel, A., López, M., Managau, S., Mann, R., Mantelet, G., Marchal, O., Marchant, J., Marconi, M., Marinoni, S., Marschalkó, G., Marshall, D., Martino, M., Marton, G., Mary, N., Massari, D., Matijevič, G., Mazeh, T., McMillan, P., Messina, S., Michalik, D., Millar, N., Molina, D., Molinaro, R., Molnár, L., Montegriffo, P., Mor, R., Morbidelli, R., Morel, T., Morris, D., Mulone, A., Muraveva, T., Musella, I., Nelemans, G., Nicastro, L., Noval, L., O'Mullane, W., Ordénovic, C., Ordóñez-Blanco, D., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Panahi, A., Pawlak, M., Piersimoni, A., Pineau, F., Plachy, E., Plum, G., Poggio, E., Poujoulet, E., Prša, A., Pulone, L., Racero, E., Ragaini, S., Rambaux, N., Ramos-Lerate, M., Regibo, S., Reylé, C., Riclet, F., Ripepi, V., Riva, A., Rivard, A., Rixon, G., Roegiers, T., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sagristà Sellés, T., Sahlmann, J., Salgado, J., Salguero, E., Sanna, N., Santana-Ros, T., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J., Ségransan, D., Shih, I., Siltala, L., Silva, A., Smart, R., Smith, K., Solano, E., Solitro, F., Sordo, R., Soria Nieto, S., Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I., Steidelmüller, H., Stephenson, C., Stoev, H., Suess, F., Surdej, J., Szabados, L., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M., Teixeira, R., Terrett, D., Teyssandier, P., Thuillot, W., Titarenko, A., Torra Clotet, F., Turon, C., Ulla, A., Utrilla, E., Uzzi, S., Vaillant, M., Valentini, G., Valette, V., van Elteren, A., Van Hemelryck, E., van Leeuwen, M., Vaschetto, M., Vecchiato, A., Veljanoski, J., Viala, Y., Vicente, D., Vogt, S., von Essen, C., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Wertz, O., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Ziaeepour, H., Zorec, J., Zschocke, S., Zucker, S., Zurbach, C., Zwitter, T., Agence Spatiale Européenne = European Space Agency (ESA), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Universität Greifswald - University of Greifswald, Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (UB), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université libre de Bruxelles (ULB), Human Cancer Genetics Program, Comprehensive Cancer Center-College of Medicine and Public Health [Colombus], M2A 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Zentrum für astronomie, Universität Heidelberg [Heidelberg] = Heidelberg University, International Center for Relativistic Astrophysics (ICRA), Università degli Studi di Roma, GIGA-Neurosciences, Université de Liège, Department of Biomedical, Metabolic and Neural Sciences [Modena], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Nelson Mandela University [Port Elizabeth], University of Las Palmas de Gran Canaria (ULPGC), Heckscher-Klinikum, Departament de Geodinamica i Geofısica, Facultat de Geologia, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Professions, institutions, temporalités (PRINTEMPS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Systèmes de Référence Temps Espace (SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Maison des Agriculteurs, Association pour le Developpement de l'Apiculture Provencale (ADAPI), Université de Picardie Jules Verne (UPJV), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Groupement de Recherche et d'Etudes en Gestion à HEC (GREGH), Ecole des Hautes Etudes Commerciales (HEC Paris)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), SIM/IDL Faculdade de Ciências da Universidade de Lisboa (FCUL), University of Lisboa, Helsinki Institute of Physics (HIP), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, INAF - Osservatorio Astronomico di Bologna (OABO), Sol Agro et hydrosystème Spatialisation (SAS), Institut National de la Recherche Agronomique (INRA)-AGROCAMPUS OUEST, Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), National Institute for Subatomic Physics [Amsterdam] (NIKHEF), Department of Medicine, Icahn School of Medicine at Mount Sinai [New York] (MSSM), Department of Environmental Chemistry, IDAEA-CSIC, Institute of Environmental Assessment and Water Research (IDAEA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics and Astronomy [Leicester], University of Leicester, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université Grenoble Alpes - UFR Langage, lettres et arts du spectacle, information et communication - Dpt Lettres et arts du spectacle (UGA UFR LLASIC LAS), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), INAF - Osservatorio Astronomico di Padova (OAPD), FORMATION STELLAIRE 2018, CICEnergigune, Atotech Deutschland GmbH, Atotech, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Queen Elizabeth Hospital, Queens Elizabeth Hospital [Birmingham], Institute of Astronomy [Leuven], Hospital Israelita Albert Einstein [São Paulo, Brazil], Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Department of Computing, Electronics and Mechatronics, Universidad de las Américas [Puebla] (UDLAP), Uppsala University, Laboratoire de Spectroscopie Hertzienne de l'ENS (LSH-ENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Service de médecine interne diabète et maladies métaboliqe, Hôpital civil Strasbourg, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Aberystwyth University, Institut de Physique et Chimie des Matériaux de Strasbourg (IPCMS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National d'Études Spatiales [Toulouse] (CNES), Sciences Pour l'Oenologie (SPO), Université Montpellier 1 (UM1)-Institut National de la Recherche Agronomique (INRA)-Université de Montpellier (UM)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Department of Physics [Athens], National and Kapodistrian University of Athens (NKUA), Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), DEE, Budapest University of Technology and Economics [Budapest] (BME), European Space Astronomy Centre (ESAC), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ingienerie des Polymères pour les Hautes Technologies (LIPHT), Ecole européenne de chimie, polymères et matériaux [Strasbourg]-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Leibniz-Institut für Astrophysik Potsdam (AIP), Atmel Corporation (ATMEL), ATMEL, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, TKK Helsinki University of Technology (TKK), Laboratoire de Recherche sur la Réactivité des Solides (LRRS), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Tel Aviv] (TAU), Raymond and Beverly Sackler Faculty of Exact Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU)-Tel Aviv University (TAU), Centre for Integrative Physiology, University of Edinburgh, Istituto Nazionale di Astrofisica (Istituto Nazionale di Astrofisica), Istituto Nazionale di Fisica Nucleare (INFN), Diagnostic Imaging and Research Institute, University of Toronto, Centre Atlantique de Philosophie (CAPHI), PRES Université Nantes Angers Le Mans (UNAM), Service de Neurologie [Hôpitaux Civils de Colmar], Hôpitaux Civils Colmar, Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), INAF - Osservatorio Astronomico di Capodimonte (OAC), Institut de recherche de l'European Business School (IREBS), European Business School Paris (EBS Paris), Département Réseaux, Information, Multimédia (RIM-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Centre G2I, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Biochemical and Chemical Engineering, Technische Universität Dortmund [Dortmund] (TU), Centre de recherche en linguistique et traitement automatique des langues, Lucien Tesnière - UFC (EA 2283) (TESNIERE), Université de Franche-Comté (UFC), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Université Paris 1 Panthéon-Sorbonne - UFR d'Économie (UP1 UFR02), Université Paris 1 Panthéon-Sorbonne (UP1), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), Spanish Virtual Observatory - Observatorio Virtual Español, Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, Institut d'Astrophysique et de Géophysique [Liège], Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), Center for health studies, Dipartimento di Fisica, Politecnico di Milano [Milan] (POLIMI), Ecologie, Evolution, Symbiose (EES), Ecologie et biologie des interactions (EBI), Université de Poitiers-Centre National de la Recherche Scientifique (CNRS)-Université de Poitiers-Centre National de la Recherche Scientifique (CNRS), Astrometry, Istituto Nazionale di Astrofisica (INAF)-Istituto Nazionale di Astrofisica (INAF), Karl-Franzens-Universität Graz, Herpetological Section, Zoologisches Forschungsmuseum Alexander Koenig, Institute of Hydrology, Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Laboratoire de l'Accélérateur Linéaire (LAL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Lohrmann Observatory, Technische Universität Dresden = Dresden University of Technology (TU Dresden), Ben-Gurion University of the Negev (BGU), Kapteyn Astronomical Institute, Astronomy, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels], Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées, Solvay Silica, Solvay (France), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, École normale supérieure - Paris (ENS Paris), Agence Spatiale Européenne (ESA), European Space Agency (ESA), University of Geneva [Switzerland], Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg], Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Genève (UNIGE), Association pour le Développement de l'Apiculture Provençale (ADAPI), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Helsinki, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), AUTRES, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Hospital Israelita Albert Einstein, Centre d'Immunologie et de Maladies Infectieuses (CIMI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Université Montpellier 1 (UM1)-Université de Montpellier (UM)-Institut National de la Recherche Agronomique (INRA), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Carnegie Institution for Science [Washington], Universidade de São Paulo (USP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Universidad de Cantabria, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Pomies, Marie-Paule, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro)-Université Montpellier 1 (UM1)-Université de Montpellier (UM)-Institut National de la Recherche Agronomique (INRA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Sciences et Technologies - Bordeaux 1, ITA, USA, GBR, FRA, DEU, ESP, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Libre de Bruxelles [Bruxelles] (ULB), PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Università di Bologna [Bologna] (UNIBO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Bologna (OABO), AGROCAMPUS OUEST-Institut National de la Recherche Agronomique (INRA), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), Spanish National Research Council (CSIC), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), observatoire astronomique de strasbourg, Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' [Rome], Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Matériaux et nanosciences d'Alsace, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), Université Montpellier 1 (UM1)-Institut de Recherche pour le Développement (IRD [Nouvelle-Calédonie])-Institut National de la Recherche Agronomique (INRA)-Université de Montpellier (UM)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, National Institute for Nuclear Physics (INFN), Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Université Panthéon-Sorbonne - UFR d'Économie (UP1 UFR02), Université Panthéon-Sorbonne (UP1), Instituto de Astronomia, Geofisica e Ciencias Atmosfericas [Sao Paulo] (IAG), Technische Universität Dresden (TUD), and Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
SKY SURVEY 2MASS, Astronomy, catalogs, astrometry, techniques: radial velocities, stars: fundamental parameters, stars: variables: general, minor planets, asteroids: general, Astrophysics, minor planets, asteroids: general, 01 natural sciences, Catàlegs d'estels, variables: general [Stars], Star catalogs, techniques: radial velocities, 010303 astronomy & astrophysics, Physics, Astrometry, CATALOG, Asteroids, asteroids: general, Radial velocity, stars: variables: general, Physical Sciences, astrometry, stars: fundamental parameters, Astrophysics - Instrumentation and Methods for Astrophysics, general [minor planets, asteroids], Asteroides, Proper motion, Vista Variables in the Via Lactea, Astrometria, DATABASE, FOS: Physical sciences, Photometric system, Astronomy & Astrophysics, fundamental parameters [Stars], Photometry (optics), [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Apparent magnitude, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, catalogs, minor planets, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysique, Science & Technology, radial velocities [Techniques], 010308 nuclear & particles physics, Minor planets, Astronomy and Astrophysics, Astronomie, Astrophysics - Astrophysics of Galaxies, Stars, Galaxy, EVOLUÇÃO ESTELAR, Estels, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Gaia Data Release 2. Summary of the contents and survey properties, Catalogs, SKY, general [Asteroids], STARS
Abstract

Context. We present the second Gaia data release, Gaia DR2, consisting of astrometry, photometry, radial velocities, and information on astrophysical parameters and variability, for sources brighter than magnitude 21. In addition epoch astrometry and photometry are provided for a modest sample of minor planets in the solar system. Aims. A summary of the contents of Gaia DR2 is presented, accompanied by a discussion on the differences with respect to Gaia DR1 and an overview of the main limitations which are still present in the survey. Recommendations are made on the responsible use of Gaia DR2 results. Methods. The raw data collected with the Gaia instruments during the first 22 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into this second data release, which represents a major advance with respect to Gaia DR1 in terms of completeness, performance, and richness of the data products. Results. Gaia DR2 contains celestial positions and the apparent brightness in G for approximately 1.7 billion sources. For 1.3 billion of those sources, parallaxes and proper motions are in addition available. The sample of sources for which variability information is provided is expanded to 0.5 million stars. This data release contains four new elements: broad-band colour information in the form of the apparent brightness in the GBP (330-680 nm) and GRP (630-1050 nm) bands is available for 1.4 billion sources; median radial velocities for some 7 million sources are presented; for between 77 and 161 million sources estimates are provided of the stellar effective temperature, extinction, reddening, and radius and luminosity; and for a pre-selected list of 14 000 minor planets in the solar system epoch astrometry and photometry are presented. Finally, Gaia DR2 also represents a new materialisation of the celestial reference frame in the optical, the Gaia-CRF2, which is the first optical reference frame based solely on extragalactic sources. There are notable changes in the photometric system and the catalogue source list with respect to Gaia DR1, and we stress the need to consider the two data releases as independent. Conclusions. Gaia DR2 represents a major achievement for the Gaia mission, delivering on the long standing promise to provide parallaxes and proper motions for over 1 billion stars, and representing a first step in the availability of complementary radial velocity and source astrophysical information for a sample of stars in the Gaia survey which covers a very substantial fraction of the volume of our galaxy., 0, info:eu-repo/semantics/published

Published
2018

25. Simulations of Effects of Nanophase Iron Space Weather Products on Lunar Regolith Reflectance Spectra

Author

Tomas Kohout, Antti Penttilä, Olga Muñoz, J. Escobar-Cerezo, Karri Muinonen, F. Moreno, Ministerio de Economía y Competitividad (España), European Commission, Academy of Finland, Ministry of Education, Youth and Sports (Czech Republic), Academy of Sciences of the Czech Republic, Particle Physics and Astrophysics, Planetary-system research, and Department of Physics

Subjects
010504 meteorology & atmospheric sciences, Mineralogy, ASTEROIDS, planets and satellites: surfaces, 7. Clean energy, 01 natural sciences, Space weathering, Spectral line, Light scattering, Physics::Geophysics, methods: numerical, Scattering, 0103 physical sciences, PARTICLES, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, NEAR-EARTH, numerical [Methods], comets: general, FINEST FRACTION, BELT, scattering, Astrophysics::Instrumentation and Methods for Astrophysics, general [Comets], Minor planets, Astronomy and Astrophysics, ION IRRADIATION, 115 Astronomy, Space science, Ray, Regolith, asteroids: general, AIRLESS BODIES, Wavelength, 13. Climate action, Space and Planetary Science, Physics::Space Physics, OLIVINE, minor planets, Lunar soil, MERCURY, surfaces [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, general [Asteroids]
Abstract

Lunar soil spectra differ from pulverized lunar rocks spectra by reddening and darkening effects, and shallower absorption bands. These effects have been described in the past as a consequence of space weathering. In this work, we focus on the effects of nanophase iron (npFe) inclusions on the experimental reflectance spectra of lunar regolith particles. The reflectance spectra are computed using SIRIS3, a code that combines ray optics with radiative-transfer modeling to simulate light scattering by different types of scatterers. The imaginary part of the refractive index as a function of wavelength of immature lunar soil is derived by comparison with the measured spectra of the corresponding material. Furthermore, the effect of adding nanophase iron inclusions on the reflectance spectra is studied. The computed spectra qualitatively reproduce the observed effects of space weathered lunar regolith. © 2018. The American Astronomical Society. All, This work has been supported by the Plan Nacional de Astronomia y Astrofisica contracts AYA2015-67152-R and AYA2015-71975-REDT. Jesus Escobar-Cerezo, Antti Penttila, and Karri Muinonen acknowledge the support from the ERC project No. 320773 >SAEMPL.> Tomas Kohout is supported by the Academy of Finland project No. 285432, and by the Institute of Geology (Czech Academy of Sciences), supported by Ministry of Education, Youth and Sports project No. RVO67985831. Computational resources were provided by CSC-IT Centre for Science Ltd, Finland.

Published
2018

26. Comparison of the orbital properties of Jupiter Trojan asteroids and Trojan dust

Author

Jürgen Schmidt and Xiaodong Liu

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, meteorites, Jupiter, Computer Science::Hardware Architecture, rings [planets and satellites], Saturn, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, meteors, meteoroids, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Meteoroid, zodiacal dust, Astronomy and Astrophysics, celestial mechanics, general [asteroids], Solar wind, Radiation pressure, solar wind, Space and Planetary Science, Asteroid, Trojan, Physics::Space Physics, minor planets, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, Astrophysics - Earth and Planetary Astrophysics
Abstract

In a previous paper we simulated the orbital evolution of dust particles from the Jupiter Trojan asteroids ejected by the impacts of interplanetary particles, and evaluated their overall configuration in the form of dust arcs. Here we compare the orbital properties of these Trojan dust particles and the Trojan asteroids. Both Trojan asteroids and most of the dust particles are trapped in the Jupiter 1:1 resonance. However, for dust particles, this resonance is modified because of the presence of solar radiation pressure, which reduces the peak value of the semi-major axis distribution. We find also that some particles can be trapped in the Saturn 1:1 resonance and higher order resonances with Jupiter. The distributions of the eccentricity, the longitude of pericenter, and the inclination for Trojans and the dust are compared. For the Trojan asteroids, the peak in the longitude of pericenter distribution is about 60 degrees larger than the longitude of pericenter of Jupiter; in contrast, for Trojan dust this difference is smaller than 60 degrees, and it decreases with decreasing grain size. For the Trojan asteroids and most of the Trojan dust, the Tisserand parameter is distributed in the range of two to three., Comment: 10 figures. See blog post about this study in http://planetary-mechanics.com/2018/04/15/dust-coorbital-to-jupiter/

Published
2018

27. On the age of the Beagle secundary asteroid family

Author

Valerio Carruba and Universidade Estadual Paulista (Unesp)

Subjects
Physics, Zodiacal light, 010504 meteorology & atmospheric sciences, myr, Minor planets, Astronomy and Astrophysics, Astrophysics, Asteroid family, 01 natural sciences, Beagle, Celestial mechanics, Ejection velocity, individual: (656) Beagle [Asteroids], Space and Planetary Science, Asteroid, 0103 physical sciences, Longitude, 010303 astronomy & astrophysics, general [Asteroids], 0105 earth and related environmental sciences
Abstract

Made available in DSpace on 2018-12-11T17:38:27Z (GMT). No. of bitstreams: 0 Previous issue date: 2018-01-01 California Institute of Technology Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) The Beagle family is a C-type subgroup of the Themis family, in the outer main belt. Previous works suggested that it could be younger than 20 Myr and a possible source for the dust in the i≃1.4∘ α zodiacal dust band. Here we took advantage of a much larger database for Beagle family members to revisit previous age estimates of this group. Standard dating techniques based on the family V-shape or on Monte Carlo methods of Yarkovsky and YORP mobility suggest that i) there might be a dichotomy for the inner and outer part of the Beagle family, which may be either two separate families or the product of an anisotropic ejection velocity field and that ii) the age of the possibly younger outer part of the Beagle family should be 35−35 +65 Myr. The past convergence of Beagle longitude of the node is compatible with a family age of ≃14 Myr, when (1678) Glarona is used as a reference orbit. Without further information on Beagle members spin states, however, only very lower limits on the family age can be currently obtained when the Yarkovksy force is accounted for. São Paulo State University (UNESP) School of Natural Sciences and Engineering São Paulo State University (UNESP) School of Natural Sciences and Engineering CNPq: 305453/2011-4

Published
2018

28. Extreme asteroids in the Pan-STARRS 1 Survey

Author

Andrew McNeill, Christopher A. Watson, David E. Trilling, Eva Lilly, Alan Fitzsimmons, A. Thompson, Ernst DeMooij, Pedro Lacerda, Matthew J. Hooton, and Robert Jedicke

Subjects
Physics, Rotation period, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Retrograde motion, observational [methods], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Lambda, Light curve, 01 natural sciences, general [asteroids], photometric [techniques], Amplitude, Space and Planetary Science, Asteroid, 0103 physical sciences, minor planets, Beta (velocity), 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Spin-½
Abstract

Using the first 18 months of the Pan-STARRS 1 survey we have identified 33 candidate high-amplitude objects for follow-up observations and carried out observations of 22 asteroids. 4 of the observed objects were found to have observed amplitude $A_{obs}\geq 1.0$ mag. We find that these high amplitude objects are most simply explained by single rubble pile objects with some density-dependent internal strength, allowing them to resist mass shedding even at their highly elongated shapes. 3 further objects although below the cut-off for 'high-amplitude' had a combination of elongation and rotation period which also may require internal cohesive strength, depending on the density of the body. We find that none of the 'high-amplitude asteroids' identified here require any unusual cohesive strengths to resist rotational fission. 3 asteroids were sufficiently observed to allow for shape and spin pole models to be determined through light curve inversion. 45864 was determined to have retrograde rotation with spin pole axes $\lambda=218\pm 10^{\circ}, \beta=-82\pm 5^{\circ}$ and asteroid 206167 was found to have best fit spin pole axes $\lambda= 57 \pm 5^{\circ}$, $\beta=-67 \pm 5^{\circ}$. An additional object not initially measured with $A_{obs}>1.0$ mag, 49257, was determined to have a shape model which does suggest a high-amplitude object. Its spin pole axes were best fit for values $\lambda=112\pm 6^{\circ}, \beta=6\pm 5^{\circ}$. In the course of this project to date no large super-fast rotators ($P_{rot} < 2.2$ h) have been identified., Comment: 31 pages; accepted by AJ

Published
2018
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29. Gaia Data Release 2 : Observations of solar system objects

Author

Collaboration, G., Spoto, F., Tanga, P., Mignard, F., Berthier, J., Carry, B., Cellino, A., Dell'Oro, A., Hestroffer, D., Muinonen, K., Pauwels, T., Petit, J., David, P., De Angeli, F., Delbo, M., Frézouls, B., Galluccio, L., Granvik, M., Guiraud, J., Hernández, J., Ordénovic, C., Portell, J., Poujoulet, E., Thuillot, W., Walmsley, G., Brown, A., Vallenari, A., Prusti, T., de Bruijne, J., Babusiaux, C., Bailer-Jones, C., Biermann, M., Evans, D., Eyer, L., Jansen, F., Jordi, C., Klioner, S., Lammers, U., Lindegren, L., Luri, X., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H., Soubiran, C., van Leeuwen, F., Walton, N., Arenou, F., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Lattanzi, M., Bakker, J., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., Fabricius, C., Guerra, R., Holl, B., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Panuzzo, P., Riello, M., Seabroke, G., Thévenin, F., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Teyssier, D., Altmann, M., Andrae, R., Audard, M., Bellas-Velidis, I., Benson, K., Blomme, R., Burgess, P., Busso, G., Clementini, G., Clotet, M., Creevey, O., Davidson, M., De Ridder, J., Delchambre, L., Ducourant, C., Fernández-Hernández, J., Fouesneau, M., Frémat, Y., García-Torres, M., González-Núñez, J., González-Vidal, J., Gosset, E., Guy, L., Halbwachs, J., Hambly, N., Harrison, D., Hodgkin, S., Hutton, A., Jasniewicz, G., Jean-Antoine-Piccolo, A., Jordan, S., Korn, A., Krone-Martins, A., Lanzafame, A., Lebzelter, T., Lö, W., Manteiga, M., Marrese, P., Martín-Fleitas, J., Moitinho, A., Mora, A., Osinde, J., Pancino, E., Recio-Blanco, A., Richards, P., Rimoldini, L., Robin, A., Sarro, L., Siopis, C., Smith, M., Sozzetti, A., Süveges, M., Torra, J., van Reeven, W., Abbas, U., Abreu Aramburu, A., Accart, S., Aerts, C., Altavilla, G., Álvarez, M., Alvarez, R., Alves, J., Anderson, R., Andrei, A., Anglada Varela, E., Antiche, E., Antoja, T., Arcay, B., Astraatmadja, T., Bach, N., Baker, S., Balaguer-Núñez, L., Balm, P., Barache, C., Barata, C., Barbato, D., Barblan, F., Barklem, P., Barrado, D., Barros, M., Barstow, M., Bartholomé Muñoz, L., Bassilana, J., Becciani, U., Bellazzini, M., Berihuete, A., Bertone, S., Bianchi, L., Bienaymé, O., Blanco-Cuaresma, S., Boch, T., Boeche, C., Bombrun, A., Borrachero, R., Bossini, D., Bouquillon, S., Bourda, G., Bragaglia, A., Bramante, L., Breddels, M., Bressan, A., Brouillet, N., Brüsemeister, T., Brugaletta, E., Bucciarelli, B., Burlacu, A., Busonero, D., Butkevich, A., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzaro, G., Cantat-Gaudin, T., Carballo, R., Carlucci, T., Carrasco, J., Casamiquela, L., Castellani, M., Castro-Ginard, A., Charlot, P., Chemin, L., Chiavassa, A., Cocozza, G., Costigan, G., Cowell, S., Crifo, F., Crosta, M., Crowley, C., Cuypers, J., Dafonte, C., Damerdji, Y., Dapergolas, A., David, M., de Laverny, P., De Luise, F., De March, R., de Souza, R., de Torres, A., Debosscher, J., del Pozo, E., Delgado, A., Delgado, H., Diakite, S., Diener, C., Distefano, E., Dolding, C., Drazinos, P., Durán, J., Edvardsson, B., Enke, H., Eriksson, K., Esquej, P., Eynard Bontemps, G., Fabre, C., Fabrizio, M., Faigler, S., Falcão, A., Farràs Casas, M., Federici, L., Fedorets, G., Fernique, P., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fraile, E., Fraser, M., Gai, M., Galleti, S., Garabato, D., García-Sedano, F., Garofalo, A., Garralda, N., Gavel, A., Gavras, P., Gerssen, J., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Glass, F., Gomes, M., Gueguen, A., Guerrier, A., Gutié, R., Haigron, R., Hatzidimitriou, D., Hauser, M., Haywood, M., Heiter, U., Helmi, A., Heu, J., Hilger, T., Hobbs, D., Hofmann, W., Holland, G., Huckle, H., Hypki, A., Icardi, V., Janßen, K., Jevardat de Fombelle, G., Jonker, P., Juhász, Á., Julbe, F., Karampelas, A., Kewley, A., Klar, J., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, M., Kontizas, E., Koposov, S., Kordopatis, G., Kostrzewa-Rutkowska, Z., Koubsky, P., Lambert, S., Lanza, A., Lasne, Y., Lavigne, J., Le Fustec, Y., Le Poncin-Lafitte, C., Lebreton, Y., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H., Lister, T., Livanou, E., Lobel, A., López, M., Managau, S., Mann, R., Mantelet, G., Marchal, O., Marchant, J., Marconi, M., Marinoni, S., Marschalkó, G., Marshall, D., Martino, M., Marton, G., Mary, N., Massari, D., Matijevič, G., Mazeh, T., McMillan, P., Messina, S., Michalik, D., Millar, N., Molina, D., Molinaro, R., Molnár, L., Montegriffo, P., Mor, R., Morbidelli, R., Morel, T., Morris, D., Mulone, A., Muraveva, T., Musella, I., Nelemans, G., Nicastro, L., Noval, L., O'Mullane, W., Ordóñez-Blanco, D., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Panahi, A., Pawlak, M., Piersimoni, A., Pineau, F., Plachy, E., Plum, G., Poggio, E., Prša, A., Pulone, L., Racero, E., Ragaini, S., Rambaux, N., Ramos-Lerate, M., Regibo, S., Reylé, C., Riclet, F., Ripepi, V., Riva, A., Rivard, A., Rixon, G., Roegiers, T., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sagristà Sellés, T., Sahlmann, J., Salgado, J., Salguero, E., Sanna, N., Santana-Ros, T., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J., Ségransan, D., Shih, I., Siltala, L., Silva, A., Smart, R., Smith, K., Solano, E., Solitro, F., Sordo, R., Soria Nieto, S., Souchay, J., Spagna, A., Stampa, U., Steele, I., Steidelmüller, H., Stephenson, C., Stoev, H., Suess, F., Surdej, J., Szabados, L., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M., Teixeira, R., Terrett, D., Teyssandier, P., Titarenko, A., Torra Clotet, F., Turon, C., Ulla, A., Utrilla, E., Uzzi, S., Vaillant, M., Valentini, G., Valette, V., van Elteren, A., Van Hemelryck, E., van Leeuwen, M., Vaschetto, M., Vecchiato, A., Veljanoski, J., Viala, Y., Vicente, D., Vogt, S., von Essen, C., Voss, H., Votruba, V., Voutsinas, S., Weiler, M., Wertz, O., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Ziaeepour, H., Zorec, J., Zschocke, S., Zucker, S., Zurbach, C., Zwitter, T., Universidad de Cantabria, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Helsinki Institute of Physics (HIP), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Royal Observatory of Belgium [Brussels] (ROB), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Agence Spatiale Européenne = European Space Agency (ESA), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (UB), Université libre de Bruxelles (ULB), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Zentrum für astronomie, Universität Heidelberg [Heidelberg] = Heidelberg University, University of Las Palmas de Gran Canaria (ULPGC), Departament de Geodinamica i Geofısica, Facultat de Geologia, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Systèmes de Référence Temps Espace (SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Picardie Jules Verne (UPJV), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), SIM/IDL Faculdade de Ciências da Universidade de Lisboa (FCUL), University of Lisboa, INAF - Osservatorio Astronomico di Bologna (OABO), National Institute for Subatomic Physics [Amsterdam] (NIKHEF), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics and Astronomy [Leicester], University of Leicester, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), INAF - Osservatorio Astronomico di Padova (OAPD), FORMATION STELLAIRE 2018, Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CICEnergigune, Atotech Deutschland GmbH, Atotech, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Uppsala University, Laboratoire de Spectroscopie Hertzienne de l'ENS (LSH-ENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Service de médecine interne diabète et maladies métaboliqe, Hôpital civil Strasbourg, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Aberystwyth University, Centre National d'Études Spatiales [Toulouse] (CNES), Department of Physics [Athens], National and Kapodistrian University of Athens (NKUA), Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), DEE, Budapest University of Technology and Economics [Budapest] (BME), European Space Astronomy Centre (ESAC), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Leibniz-Institut für Astrophysik Potsdam (AIP), Atmel Corporation (ATMEL), ATMEL, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), TKK Helsinki University of Technology (TKK), School of Physics and Astronomy [Tel Aviv] (TAU), Raymond and Beverly Sackler Faculty of Exact Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU)-Tel Aviv University (TAU), Istituto Nazionale di Astrofisica (Istituto Nazionale di Astrofisica), Istituto Nazionale di Fisica Nucleare (INFN), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), INAF - Osservatorio Astronomico di Capodimonte (OAC), Institut de recherche de l'European Business School (IREBS), European Business School Paris (EBS Paris), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), Spanish Virtual Observatory - Observatorio Virtual Español, Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), Dipartimento di Fisica, Politecnico di Milano [Milan] (POLIMI), Astrometry, Istituto Nazionale di Astrofisica (INAF)-Istituto Nazionale di Astrofisica (INAF), Karl-Franzens-Universität Graz, Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Laboratoire de l'Accélérateur Linéaire (LAL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Lohrmann Observatory, Technische Universität Dresden = Dresden University of Technology (TU Dresden), Ben-Gurion University of the Negev (BGU), Department of Physics, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Helsinki, Royal Observatory of Belgium [Brussels], Agence Spatiale Européenne (ESA), European Space Agency (ESA), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), University of Geneva [Switzerland], Université Libre de Bruxelles [Bruxelles] (ULB), Universität Heidelberg [Heidelberg], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), Università di Bologna [Bologna] (UNIBO), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Bologna (OABO), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), observatoire astronomique de strasbourg, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre d'Immunologie et de Maladies Infectieuses (CIMI), Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' [Rome], National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], National Institute for Nuclear Physics (INFN), Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Carnegie Institution for Science [Washington], Instituto de Astronomia, Geofisica e Ciencias Atmosfericas [Sao Paulo] (IAG), Universidade de São Paulo (USP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Technische Universität Dresden (TUD), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Kapteyn Astronomical Institute, Astronomy, ITA, GBR, FRA, DEU, ESP, BEL, Pomies, Marie-Paule, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Gaia Collaboration

Subjects
Solar System, Brightness, instruments [space vehicles], 010504 meteorology & atmospheric sciences, Computer science, Astronomy, ASTEROIDS, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, law.invention, astrometry, minor planets, asteroids: general, methods: data analysis, space vehicles, instruments, astrophysics, earth and planetary astrophysics, astrophysics - instrumentation and methods for astrophysics, Astronomi, astrofysik och kosmologi, law, Astronomy, Astrophysics and Cosmology, INVERSION, Space vehicles: instruments, 010303 astronomy & astrophysics, QC, QB, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Physics, 520 Astronomy, Astrometry, SCIENCE, Asteroids, Data processing, Asteroid, ASTROMETRIA, Physical Sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Système solaire, general [minor planets, asteroids], Asteroides, space vehicles: instruments, FOS: Physical sciences, Astronomy & Astrophysics, Photometry (optics), [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Apparent magnitude, Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, 0103 physical sciences, data analysis [methods], PHOTOMETRY, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysique, Minor planet, 0105 earth and related environmental sciences, Science & Technology, Astronomy and Astrophysics, Photometer, Astronomie, 115 Astronomy, Space science, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], general [asteroids], Space and Planetary Science, Minor planets, asteroids: general, Astrophysics - Earth and Planetary Astrophysics, Processament de dades
Abstract

Context. The Gaia spacecraft of the European Space Agency (ESA) has been securing observations of solar system objects (SSOs) since the beginning of its operations. Data Release 2 (DR2) contains the observations of a selected sample of 14,099 SSOs. These asteroids have been already identified and have been numbered by the Minor Planet Center repository. Positions are provided for each Gaia observation at CCD level. As additional information, complementary to astrometry, the apparent brightness of SSOs in the unfiltered G band is also provided for selected observations. Aims. We explain the processing of SSO data, and describe the criteria we used to select the sample published in Gaia DR2. We then explore the data set to assess its quality. Methods. To exploit the main data product for the solar system in Gaia DR2, which is the epoch astrometry of asteroids, it is necessary to take into account the unusual properties of the uncertainty, as the position information is nearly one-dimensional. When this aspect is handled appropriately, an orbit fit can be obtained with post-fit residuals that are overall consistent with the a-priori error model that was used to define individual values of the astrometric uncertainty. The role of both random and systematic errors is described. The distribution of residuals allowed us to identify possible contaminants in the data set (such as stars). Photometry in the G band was compared to computed values from reference asteroid shapes and to the flux registered at the corresponding epochs by the red and blue photometers (RP and BP). Results. The overall astrometric performance is close to the expectations, with an optimal range of brightness G ∼ 12 - 17. In this range, the typical transit-level accuracy is well below 1 mas. For fainter asteroids, the growing photon noise deteriorates the performance. Asteroids brighter than G ∼ 12 are affected by a lower performance of the processing of their signals. The dramatic improvement brought by Gaia DR2 astrometry of SSOs is demonstrated by comparisons to the archive data and by preliminary tests on the detection of subtle non-gravitational effects., 0, info:eu-repo/semantics/published

Published
2018

30. The resonant population of asteroids in librating states of the ν 6 linear secular resonance

Author

R. C. Domingos, M. Huaman, Valerio Carruba, Safwan Aljbaae, Fernando Roig, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), FEG/UNESP, Systèmes de Référence Temps Espace (SYRTE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Pesquisas Espaciais (INPE), Ministério da Ciência, Tecnologia e Inovação, Observatório Nacional (ON), and Universidade Estadual Paulista (Unesp)

Subjects
Physics, education.field_of_study, 010504 meteorology & atmospheric sciences, Population, Astronomy, Minor planets, Astronomy and Astrophysics, 01 natural sciences, Celestial mechanics, Secular resonance, Space and Planetary Science, Asteroid, 0103 physical sciences, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, general [Asteroids], 0105 earth and related environmental sciences
Abstract

Made available in DSpace on 2019-10-06T17:01:43Z (GMT). No. of bitstreams: 0 Previous issue date: 2018-12-01 We discuss the asteroid population evolving close by or into the υ6 secular resonance in the main asteroid belt. Using the analytical method of Yoshikawa, we estimate the actual domain of the υ6 resonance, which currently contains 4 137 asteroids identified from the AstDys catalogue.We perform numerical integrations of the obits of these asteroids, considering the gravitational perturbation of all the planets, and identify those showing pure libration states. For the first time, seven asteroids are found to librate in aligned states, all located at the central main belt. We analyse the stability of this new population by extending our numerical integrations both into the past and into the future, to find that all of them are stable, but only four of them display long-term aligned librations. We also identified the asteroid families located close to and within the domain of the υ6 secular resonance, with a particular focus on the Svea family, which has 54 per cent of its members librating in anti-aligned states. This is the third family identified to be largely affected by the υ6 resonance, together with the families of Tina and Euphrosyne. Observatório Nacional (ON), Rua Gal. Jose Cristino 77 São Paulo State University (UNESP) School of Natural Sciences and Engineering São Paulo State University (UNESP), Campus of São São Paulo State University (UNESP) School of Natural Sciences and Engineering São Paulo State University (UNESP), Campus of São

Published
2018

31. On the calibration of the relation between geometric albedo and polarimetric properties for the asteroids

Author

M. Canada-Assandri, Edward F. Tedesco, Alberto Cellino, Stefano Bagnulo, Ricardo Gil-Hutton, and Paolo Tanga

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), POLARIMETRIC [TECHNIQUES], Physics, Ciencias Físicas, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], GENERAL [ASTEROIDS], purl.org/becyt/ford/1 [https], Astronomía, MINOR PLANETS, Space and Planetary Science, Asteroid, Geometric albedo, Astrophysics::Earth and Planetary Astrophysics, CIENCIAS NATURALES Y EXACTAS, Physics::Atmospheric and Oceanic Physics, Astrophysics - Earth and Planetary Astrophysics, Remote sensing
Abstract

We present a new extensive analysis of the old problem of finding a satisfactory calibration of the relation between the geometric albedo and some measurable polarization properties of the asteroids. To achieve our goals, we use all polarimetric data at our disposal. For the purposes of calibration, we use a limited sample of objects for which we can be confident to know the albedo with good accuracy, according to previous investigations of other authors. We find a new set of updated calibration coefficients for the classical slope - albedo relation, but we generalize our analysis and we consider also alternative possibilities, including the use of other polarimetric parameters, one being proposed here for the first time, and the possibility to exclude from best-fit analyzes the asteroids having low albedos. We also consider a possible parabolic fit of the whole set of data., Accepted by MNRAS

Published
2015

32. Prospects of Dynamical Determination of General Relativity Parameter β and Solar Quadrupole Moment J(2 circle dot) with Asteroid Radar Astronomy

Author

Verma, Ashok K, Margot, Jean-Luc, and Greenberg, Adam H

Subjects
parameters, gr-qc, Molecular, Astronomy & Astrophysics, Atomic, general [asteroids], Particle and Plasma Physics, gravitation, radar astronomy [techniques], physics.space-ph, Physics::Space Physics, fundamental [Sun], astro-ph.EP, minor planets, astrometry, Nuclear, Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences, relativistic processes, Physical Chemistry (incl. Structural)
Abstract

We evaluated the prospects of quantifying the parameterized post-Newtonian parameter beta and solar quadrupole moment J2 with observations of near-Earth asteroids with large orbital precession rates (9 to 27 arcsec century$^{-1}$). We considered existing optical and radar astrometry, as well as radar astrometry that can realistically be obtained with the Arecibo planetary radar in the next five years. Our sensitivity calculations relied on a traditional covariance analysis and Monte Carlo simulations. We found that independent estimates of beta and J2 can be obtained with precisions of $6\times10^{-4}$ and $3\times10^{-8}$, respectively. Because we assumed rather conservative observational uncertainties, as is the usual practice when reporting radar astrometry, it is likely that the actual precision will be closer to $2\times10^{-4}$ and $10^{-8}$, respectively. A purely dynamical determination of solar oblateness with asteroid radar astronomy may therefore rival the helioseismology determination.

Published
2017

34. Formation of Pebble-Pile Planetesimals and the Interior Structure of Comets

Author

Wahlberg Jansson, Karl

Subjects
minor planets, Astronomy, Astrophysics and Cosmology, formation [planets and satellites], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, general [asteroids], general [comets]
Abstract

Planets form in protoplanetary discs of gas, dust and ice around newborn stars. In the Solar System, not only planets are found as a result from the time of planet formation, but also remnant planetesimals in the form of asteroids, Kuiper belt objects and comets. Recent observations, e.g. by the space mission Rosetta, have found that comets are porous objects barely able to hold themselves together by gravity.Gravitationally bound clouds of mm- to dm-sized pebbles can form in the protoplanetary disc by interactions between solids and the gas, e.g. through the streaming instability. Such clouds will have collisions between pebbles resulting in energy dissipation and inevitably a collapse into a solid planetesimal.In paper I we develop a statistical model to investigate, with numerical simulations, the collapse of pebble clouds into planetesimals. We find that low-mass planetesimals, e.g. comets, are porous pebble-piles with this formation mechanism. Paper II and III investigate the role of fragmenting collisions in planetesimal formation, both with laboratory experiments and numerical simulations.The above model assumes an isolated, homogeneous planetesimal. In paper IV we find that the interior structure of comets can vary with depth ('onion'-like shells) and that gas in the protoplanetary disc can affect the collapse significantly.

Published
2017

35. Origin of slow-rotating minor bodies by tidal decoupling of binary pairs

Author

Adrian Brunini

Subjects
Physics, 010504 meteorology & atmospheric sciences, Ciencias Físicas, Binary number, Astronomy and Astrophysics, Decoupling (cosmology), Astrophysics, GENERAL [ASTEROIDS], 01 natural sciences, Astronomía, MINOR PLANETS, Space and Planetary Science, Asteroid, 0103 physical sciences, 010303 astronomy & astrophysics, CIENCIAS NATURALES Y EXACTAS, 0105 earth and related environmental sciences
Abstract

In this paper, we show that the decoupling of binary pairs by tidal interaction and Kozai oscillations acting together can generate single objects in a slow-rotation-rate state. This mechanism has the merit of not being strongly dependent on the size or shape of the objects. The key parameter leading the process is ω/n, the ratio between the rotation rate and the orbital mean motion of the binary, which must be > 1. The proposed mechanism could also operate in other populations of minor bodies. Fil: Brunini, Adrian. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de la Patagonia Austral. Unidad Académica Caleta Olivia. Departamento de Ciencias Exactas y Naturales; Argentina

Published
2017

36. Evolution of Occator Crater on (1) Ceres

Author

Vishnu Reddy, Edward A. Cloutis, Guneshwar Thangjam, Kurt Mengel, Andreas Nathues, Thomas Platz, David A. Crown, L. Le Corre, Martin Hoffmann, and J. Kallisch

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, language.human_language, general [asteroids], German, symbols.namesake, Impact crater, Space and Planetary Science, Asteroid, 0103 physical sciences, language, symbols, minor planets, Planck, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The dwarf planet Ceres (diameter 939 km) is the largest object in the main asteroid belt. Recent investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential geological activity, a body which was never completely molten but possibly differentiated into a rocky core, an ice-rich mantle, and which may contain remnant internal liquid water. Thermal alteration and exogenic material infall contribute to producing a (dark) carbonaceous chondritic-like surface containing ammoniated phyllosilicates. Here we report imaging and spectroscopic analyses of Occator crater derived from the Framing Camera and the Visible and Infrared Spectrometer onboard Dawn. We found that the central bright spot (Cerealia Facula) of Occator is ∼30 Myr younger than the crater itself. The central spot is located in a central pit which contains a dome that is spectrally homogenous, exhibiting absorption features that are consistent with carbonates. Multiple radial fractures across the dome indicate an extrusive formation process. Our results lead us to conclude that the floor region was subject to past endogenic activity. Dome and bright material in its vicinity formed likely due to a long-lasting, periodic, or episodic ascent of bright material from a subsurface reservoir rich in carbonates. Originally triggered by an impact event, gases, possibly dissolved from a subsurface water/brine layer, enabled material rich in carbonates to ascend through fractures and be deposited onto the surface. The Framing Camera project is financially supported by the Max Planck Society and the German Space Agency (DLR). http://iopscience.iop.org/article/10.3847/1538-3881/153/3/112/meta

Published
2017

37. Scattering V-type asteroids during the giant planets instability: A step for Jupiter, a leap for basalt

Author

David Nesvorný, Valerio Carruba, P. I. O. Brasil, Fernando Roig, Observ Nacl, Southwest Res Inst, and Universidade Estadual Paulista (Unesp)

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), dynamical evolution and stability [planets and satellites], Solar System, Near-Earth object, 010504 meteorology & atmospheric sciences, Giant planet, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, general [asteroids], Astrobiology, Jupiter, Jumping-Jupiter scenario, Space and Planetary Science, Asteroid, Planet, 0103 physical sciences, minor planets, Asteroid belt, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

V-type asteroids are a taxonomic class whose surface is associated to a basaltic composition. The only known source of V-type asteroids in the Main Asteroid Belt is (4) Vesta, that is located in the inner part of the belt. However, many V-type asteroids cannot be dynamically linked to Vesta., in particular, those asteroids located in the middle and outer parts of the Belt. Previous works have failed to find mechanisms to transport V-type asteroids from the inner to the middle and outer belt. In this work we propose a dynamical mechanism that could have acted on primordial asteroid families. We consider a model of the giant planets migration known as the jumping Jupiter model with five planets. Our study is focused on the period of 10 Myr that encompasses the instability phase of the giant planets. We show that, for different hypothetical Vesta-like paleo-families in the inner belt, the perturbations caused by the ice giant that is scattered into the asteroid belt before being ejected from the solar system, are able to scatter V-type asteroids to the middle and outer belt. Based on the orbital distribution of V-type candidates identified from the Sloan Digital Sky Survey and the VISTA Survey colours, we show that this mechanism is efficient enough provided that the hypothetical paleo-family originated from a 100 to 500 km crater excavated on the surface of (4) Vesta. This mechanism is able to explain the currently observed V-type asteroids in the middle and outer belt, with the exception of (1459) Magnya., Comment: 10 pages, 4 figures. To appear in MNRAS

Published
2017
Full Text
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38. The Maria asteroid family

Author

R. C. Domingos, Valerio Carruba, M. Huaman, Joseph R. Masiero, Safwan Aljbaae, FEG/UNESP, Systèmes de Référence Temps Espace (SYRTE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Pesquisas Espaciais (INPE), Ministério da Ciência, Tecnologia e Inovação, Universidade Estadual Paulista (Unesp), Jet Propulsion Laboratory/Caltech, and Observatório Nacional (ON)

Subjects
Physics, 010504 meteorology & atmospheric sciences, Minor planets, Astronomy and Astrophysics, Asteroid family, 01 natural sciences, Celestial mechanics, Astrobiology, Gravitation, Space and Planetary Science, Asteroid, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, general [Asteroids], 0105 earth and related environmental sciences
Abstract

Made available in DSpace on 2018-12-11T17:36:38Z (GMT). No. of bitstreams: 0 Previous issue date: 2017-01-01 Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) The Maria asteroid family is a group of S-type asteroids. Its location adjacent to the left side of the 3J:-1A mean-motion resonances could be the reason for the absence of the left side of the 'V' shape in the (a, 1/D) domain. This family can be considered as a likely source of ordinary chondrite-like material. In this work, we make use of the time dependence of the asymmetric coefficient AS describing the degree of asymmetry of the C distribution of a fictitious Maria family generated with the value of the ejection velocity parameter VEJ = 35ms-1 to obtain an age estimate of 1750 +537 -231 Myr, in good agreement with the family age found in the literature. Analysing the contribution to the near-Earth object (NEO) population, we found that about 7.6 per cent of presently known near-Earth asteroids (NEAs) have orbits similar to asteroids from the Maria family. Only ~1.7 per cent of our simulated family can stay in NEO space for more than 10 Myr, while only five asteroids become NEOs in the last 500 Myr of the simulation. São Paulo State University (UNESP) School of Natural Sciences and Engineering Jet Propulsion Laboratory/Caltech, 4800 Oak Grove Dr., MS 183-601 Universidade Estadual Paulista (UNESP) Observatório Nacional (ON), Rua Gal. Jose Cristino 77 São Paulo State University (UNESP) School of Natural Sciences and Engineering Universidade Estadual Paulista (UNESP)

Published
2017

39. The Hoffmeister asteroid family

Author

Valerio Carruba, Bojan Novaković, Safwan Aljbaae, Universidade Estadual Paulista (Unesp), University of Belgrade, FEG/UNESP, Systèmes de Référence Temps Espace (SYRTE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Pesquisas Espaciais (INPE), and Ministério da Ciência, Tecnologia e Inovação

Subjects
010504 meteorology & atmospheric sciences, Field (physics), FOS: Physical sciences, Astrophysics, 01 natural sciences, Celestialmechanics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, asteroids: individual: Hoffmeister, 10. No inequality, 010303 astronomy & astrophysics, asteroids: general -minor planets, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, celestial mechanics -minor planets, Center (category theory), Minor planets, Astronomy and Astrophysics, Asteroid family, Celestial mechanics, Secular resonance, individual: Hoffmeister [Asteroids], Distribution (mathematics), Space and Planetary Science, Asteroid, Kurtosis, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

The Hoffmeister family is a C-type group located in the central main belt. Dynamically, it is important because of its interaction with the ${\nu}_{1C}$ nodal secular resonance with Ceres, that significantly increases the dispersion in inclination of family members at lower semi-major axis. As an effect, the distribution of inclination values of the Hoffmeister family at semi-major axis lower than its center is significantly leptokurtic, and this can be used to set constraints on the terminal ejection velocity field of the family at the time it was produced. By performing an analysis of the time behaviour of the kurtosis of the $v_W$ component of the ejection velocity field (${\gamma}_2(v_W)$), as obtained from Gauss' equations, for different fictitious Hoffmeister families with different values of the ejection velocity field, we were able to exclude that the Hoffmeister family should be older than 335 Myr. Constraints from the currently observed inclination distribution of the Hoffmeister family suggest that its terminal ejection velocity parameter $V_{EJ}$ should be lower than 25~m/s. Results of a Yarko-YORP Monte Carlo method to family dating, combined with other constraints from inclinations and ${\gamma}_2(v_W)$, indicate that the Hoffmeister family should be $220^{+60}_{-40}$~Myr old, with an ejection parameter $V_{EJ}= 20\pm5$~m/s., Comment: 8 pages, 7 figures. Accepted for publication in MNRAS. arXiv admin note: text overlap with arXiv:1606.05189

Published
2017

40. The Dark Energy Survey: more than dark energy – an overview

Author

Abbott, T, Abdalla, FB, Aleksić, J, Allam, S, Amara, A, Bacon, D, Balbinot, E, Banerji, M, Bechtol, K, Benoit-Lévy, A, Bernstein, GM, Bertin, E, Blazek, J, Bonnett, C, Bridle, S, Brooks, D, Brunner, RJ, Buckley-Geer, E, Burke, DL, Caminha, GB, Capozzi, D, Carlsen, J, Carnero-Rosell, A, Carollo, M, Carrasco-Kind, M, Carretero, J, Castander, FJ, Clerkin, L, Collett, T, Conselice, C, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Davis, TM, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Estrada, J, Etherington, J, Evrard, AE, Fabbri, J, Finley, DA, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Goldstein, DA, Gruen, D, Gruendl, RA, Guarnieri, P, Gutierrez, G, Hartley, W, Honscheid, K, Jain, B, James, DJ, Jeltema, T, Jouvel, S, Kessler, R, King, A, Kirk, D, Kron, R, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Makler, M, Manera, M, Maraston, C, Marshall, JL, Martini, P, McMahon, RG, Melchior, P, Merson, A, Miller, CJ, Miquel, R, Mohr, JJ, Morice-Atkinson, X, Naidoo, K, Neilsen, E, Nichol, RC, Nord, B, Ogando, R, Ostrovski, F, Palmese, A, Papadopoulos, A, Peiris, HV, Peoples, J, Percival, WJ, and Plazas, AA

Subjects
surveys, general [quasars], astro-ph.GA, minor planets, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, general [supernovae], Astrophysics::Galaxy Astrophysics, general [Galaxy], Astronomical and Space Sciences, general [asteroids], general [galaxies]
Abstract

This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and other transients. The main goals of DES are to characterize dark energy and dark matter, and to test alternative models of gravity; these goals will be pursued by studying large-scale structure, cluster counts, weak gravitational lensing and Type Ia supernovae. However, DES also provides a rich data set which allows us to study many other aspects of astrophysics. In this paper, we focus on additional science with DES, emphasizing areas where the survey makes a difference with respect to other current surveys. The paper illustrates, using early data (from 'Science Verification', and from the first, second and third seasons of observations), what DES can tell us about the Solar system, the Milky Way, galaxy evolution, quasars and other topics. In addition, we show that if the cosmological model is assumed to be Λ+cold dark matter, then important astrophysics can be deduced from the primary DES probes. Highlights from DES early data include the discovery of 34 trans-Neptunian objects, 17 dwarf satellites of the Milky Way, one published z > 6 quasar (and more confirmed) and two published superluminous supernovae (and more confirmed).

Published
2016

41. On the Astrid asteroid family

Author

Valerio Carruba and Universidade Estadual Paulista (Unesp)

Subjects
Surface (mathematics), 010504 meteorology & atmospheric sciences, Monte Carlo method, FOS: Physical sciences, Astrophysics, 01 natural sciences, individual: Astrid [Asteroids], Celestial mechanics, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Minor planets, Astronomy and Astrophysics, Asteroid family, Secular resonance, Classical mechanics, Distribution (mathematics), Space and Planetary Science, Asteroid, Kurtosis, Astrophysics::Earth and Planetary Astrophysics, general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

Among asteroid families, the Astrid family is peculiar because of its unusual inclination distribution. Objects at $a\simeq$~2.764 au are quite dispersed in this orbital element, giving the family a "crab-like" appearance. Recent works showed that this feature is caused by the interaction of the family with the $s-s_C$ nodal secular resonance with Ceres, that spreads the inclination of asteroids near its separatrix. As a consequence, the currently observed distribution of the $v_W$ component of terminal ejection velocities obtained from inverting Gauss equation is quite leptokurtic, since this parameter mostly depends on the asteroids inclination. The peculiar orbital configuration of the Astrid family can be used to set constraints on key parameters describing the strength of the Yarkovsky force, such as the bulk and surface density and the thermal conductivity of surface material. By simulating various fictitious families with different values of these parameters, and by demanding that the current value of the kurtosis of the distribution in $v_W$ be reached over the estimated lifetime of the family, we obtained that the thermal conductivity of Astrid family members should be $\simeq$ 0.001 W/m/K, and that the surface and bulk density should be higher than 1000 kg/m$^{3}$. Monte Carlo methods simulating Yarkovsky and stochastic YORP evolution of the Astrid family show its age to be $T$ = 140$\pm$30 Myr old, in good agreement with estimates from other groups. Its terminal ejection velocity parameter is in the range $V_{EJ}= 5^{+17}_{-5}$~m/s.] Values of $V_{EJ}$ larger than 25 m/s are excluded from constraints from the current inclination distribution., This paper has 8 pages and 9 figures, accepted for publication in MNRAS

Published
2016

42. Nanoindenting the Chelyabinsk meteorite to learn about impact deflection effects in asteroids

Author

Michael Küppers, Ivan Lloro, Carles E. Moyano-Cambero, Jürgen Blum, Eva Pellicer, Iwan P. Williams, Jordi Sort, Josep M. Trigo-Rodríguez, M. Martínez-Jiménez, and Patrick Michel

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Meteors, Projectile, Minor planets, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Meteoroids, Nanoindentation, 010502 geochemistry & geophysics, Kinetic energy, 01 natural sciences, Fracture toughness, Meteorite, Space and Planetary Science, Asteroid, Deflection (engineering), 0103 physical sciences, 010303 astronomy & astrophysics, general [Asteroids], Geology, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Ordinary chondrite, Meteorites
Abstract

The Chelyabinsk meteorite is a highly shocked, low porosity, ordinary chondrite, probably similar to S- or Q-type asteroids. Therefore, nanoindentation experiments on this meteorite allow us to obtain key data to understand the physical properties of near-Earth asteroids. Tests at different length scales provide information about the local mechanical properties of the minerals forming this meteorite: reduced Young's modulus, hardness, elastic recovery, and fracture toughness. Those tests are also useful to understand the potential to deflect threatening asteroids using a kinetic projectile. We found that the differences in mechanical properties between regions of the meteorite, which increase or reduce the efficiency of impacts, are not a result of compositional differences. A low mean particle size, attributed to repetitive shock, can increase hardness, while low porosity promotes a higher momentum multiplication. Momentum multiplication is the ratio between the change in momentum of a target due to an impact, and the momentum of the projectile, and, therefore higher values imply more efficient impacts. In the Chelyabinsk meteorite, the properties of the light-colored lithology materials facilitate obtaining higher momentum multiplication values, compared to the other regions described for this meteorite. Also, we found a low value of fracture toughness in the shock-melt veins of Chelyabinsk, which would promote the ejection of material after an impact and, therefore, increase the momentum multiplication. These results are relevant considering the growing interest in missions to test asteroid deflection, such as the recent collaboration between the European Space Agency and NASA, known as the Asteroid Impact and Deflection Assessment mission., Comment: 2 Tables, 4 Figures, and 19 pages in Astrophysical Journal (2017)

Published
2016
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43. Observation of two new L4 Neptune Trojans in the Dark Energy Survey supernova fields

Author

Gerdes, David W., Jennings, R. J., Bernstein, Gary M., Sako, Masao, Adams, Fred, Goldstein, Daniel Abraham, Kessler, Richard S., Hamilton, S., Abbott, Timothy M. C., Abdalla, Filipe B., Allam, Sahar S., Benoit-Lévy, Aurélien, Bertin, Emmanuel, Brooks, D., Buckley-Geer, Elizabeth, Burke, David Lyle, Capozzi, Diego, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, D'Andrea, Christopher B., Costa, Luiz N. da, DePoy, Darren L., Desai, S., Dietrich, Jörg P., Doel, Peter, Eifler, Tim, Fausti Neto, Angelo, Flaugher, Brenna, Frieman, Joshua A., Gaztañaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston R., Honscheid, K., James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Li, T. S., Maia, Marcio Antonio Geimba, March, Marisa Cristina, Martini, Paul, Miller, Christopher J., Miquel, Ramon, Nichol, Robert C., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Romer, Anita K., Roodman, Aaron, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thaler, Jon J., Walker, Alistair, Wester, William Carl, Zhang, Yuanyuan, and DES Collaboration

Subjects
Asteroides, Sistema solar, Fotometria astronômica, Minor planets, general [Asteroids]
Abstract

We report the discovery of the eighth and ninth known Trojans in stable orbits around Neptune’s leading Lagrange point, L4. The objects 2014QO441 and 2014QP441 were detected in data obtained during the 2013–14 and 2014–15 observing seasons by the Dark Energy Survey, using the Dark Energy Camera (DECam) on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory. Both are in high-inclination orbits (18°.8 and 19°.4, respectively). With an eccentricity of 0.104, 2014QO441 has the most eccentric orbit of the 11 known stable Neptune Trojans. Here we describe the search procedure and investigate the objects’ long-term dynamical stability and physical properties.

Published
2016

44. Capabilities of Earth-based radar facilities for near-Earth asteroid observations

Author

Jean-Luc Margot, Patrick A. Taylor, Lance A. M. Benner, Michael W. Busch, and Shantanu P. Naidu

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy & Astrophysics, 01 natural sciences, law.invention, Radio telescope, law, 0103 physical sciences, Radar, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Goldstone, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Near-Earth object, Green Bank Telescope, Astronomy, telescopes, Astronomy and Astrophysics, general [asteroids], Bistatic radar, radar astronomy [techniques], Space and Planetary Science, Asteroid, visual_art, astro-ph.EP, minor planets, visual_art.visual_art_medium, Antenna (radio), Astrophysics - Instrumentation and Methods for Astrophysics, Astronomical and Space Sciences, astro-ph.IM, general [minor planets, asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

We evaluated the planetary radar capabilities at Arecibo, the Goldstone 70-m DSS-14 and 34-m DSS-13 antennas, the 70-m DSS-43 antenna at Canberra, the Green Bank Telescope, and the Parkes Radio Telescope in terms of their relative sensitivities and the number of known near-Earth asteroids (NEAs) detectable per year in monostatic and bistatic configurations. In the 2015 calendar year, monostatic observations with Arecibo and DSS-14 were capable of detecting 253 and 131 NEAs respectively, with signal-to-noise ratios (SNRs) greater than 30/track. Combined, the two observatories were capable of detecting 276 NEAs. Of these, Arecibo detected 77 and Goldstone detected 32, or 30% and 24% the numbers that were possible. The two observatories detected an additional 18 and 7 NEAs respectively, with SNRs of less than 30/track. This indicates that a substantial number of potential targets are not being observed. The bistatic configuration with DSS-14 transmitting and the Green Bank Telescope receiving was capable of detecting about 195 NEAs, or ~50% more than with monostatic observations at DSS-14. Most of the detectable asteroids were targets of opportunity that were discovered less than 15 days before the end of their observing windows. About 50% of the detectable asteroids have absolute magnitudes > 25, which corresponds diameters < ~30 m., 12 pages, 7 figures, Accepted to AJ

Published
2016
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45. On the highly inclined v W leptokurtic asteroid families

Author

M. Huaman, R. C. Domingos, Valerio Carruba, Safwan Aljbaae, FEG/UNESP, Systèmes de Référence Temps Espace (SYRTE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Pesquisas Espaciais (INPE), Ministério da Ciência, Tecnologia e Inovação, and Universidade Estadual Paulista (Unesp)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Normal component, FOS: Physical sciences, Minor planets, Astronomy, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Celestial mechanics, Ejection velocity, Distribution (mathematics), Space and Planetary Science, Asteroid, Planet, 0103 physical sciences, Kurtosis, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

$v_W$ leptokurtic asteroid families are families for which the distribution of the normal component of the terminal ejection velocity field $v_W$ is characterized by a positive value of the ${\gamma}_2$ Pearson kurtosis, i.e., they have a distribution with a more concentrated peak and larger tails than the Gaussian one. Currently, eight families are known to have ${\gamma}_2(v_W) > 0.25$. Among these, three are highly inclined asteroid families, the Hansa, Barcelona, and Gallia families. As observed for the case of the Astrid family, the leptokurtic inclination distribution seems to be caused by the interaction of these families with node secular resonances. In particular, the Hansa and Gallia family are crossed by the $s-s_V$ resonance with Vesta, that significantly alters the inclination of some of their members. In this work we use the time evolution of ${\gamma}_2(v_W)$ for simulated families under the gravitational influence of all planets and the three most massive bodies in the main belt to assess the dynamical importance (or lack of) node secular resonances with Ceres, Vesta, and Pallas for the considered families, and to obtain independent constraints on the family ages. While secular resonances with massive bodies in the main belt do not significantly affect the dynamical evolution of the Barcelona family, they significantly increase the ${\gamma}_2(v_W)$ values of the simulated Hansa and Gallia families. Current values of the ${\gamma}_2(v_W)$ for the Gallia family are reached over the estimated family age only if secular resonances with Vesta are accounted for., Comment: 7 pages, 5 figures, 2 tables. Accepted for publication in MNRAS

Published
2016

46. Constraints on the original ejection velocity fields of asteroid families

Author

Valerio Carruba, David Nesvorný, Southwest Research Institute, and Universidade Estadual Paulista (Unesp)

Subjects
Orbital plane, 010504 meteorology & atmospheric sciences, Field (physics), Distribution (number theory), FOS: Physical sciences, Astrophysics, 01 natural sciences, Gravitation, 0103 physical sciences, Celestial mechanics, Flatness (cosmology), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Minor planets, Astronomy and Astrophysics, Classical mechanics, Space and Planetary Science, Asteroid, Physics::Space Physics, Kurtosis, Astrophysics::Earth and Planetary Astrophysics, general [Asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract

Asteroid families form as a result of large-scale collisions among main belt asteroids. The orbital distribution of fragments after a family-forming impact could inform us about their ejection velocities. Unfortunately, however, orbits dynamically evolve by a number of effects, including the Yarkovsky drift, chaotic diffusion, and gravitational encounters with massive asteroids, such that it is difficult to infer the ejection velocities eons after each family's formation. Here we analyze the inclination distribution of asteroid families, because proper inclination can remain constant over long time intervals, and could help us to understand the distribution of the component of the ejection velocity that is perpendicular to the orbital plane ($v_{W}$). From modeling the initial breakup, we find that the distribution of $v_{W}$ of the fragments, which manage to escape the parent body's gravity, should be more peaked than a Gaussian distribution (i.e., be leptokurtic) even if the initial distribution was Gaussian. We surveyed known asteroid families for signs of a peaked distribution of $v_{W}$ using a statistical measure of the distribution peakedness or flatness known as kurtosis. We identified eight families whose $v_{W}$ distribution is significantly leptokurtic. These cases (e.g. the Koronis family) are located in dynamically quiet regions of the main belt, where, presumably, the initial distribution of $v_{W}$ was not modified by subsequent orbital evolution. We suggest that, in these cases, the inclination distribution can be used to obtain interesting information about the original ejection velocity field., Comment: 7 pages, 5 figures, 1 table

Published
2016
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47. The collisional evolution of undifferentiated asteroids and the formation of chondritic meteoroids

Author

Jürgen Blum, E. Beitz, Josep M. Trigo-Rodríguez, and Mirta Gabriela Parisi

Subjects
Ciencias Astronómicas, planets and satellites: physical evolution, 010504 meteorology & atmospheric sciences, Ciencias Físicas, FOS: Physical sciences, Otras Ciencias Físicas, 01 natural sciences, meteorites, Astrobiology, methods: numerical, 0103 physical sciences, meteors, meteoroids, 010303 astronomy & astrophysics, planetary systems, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Meteoroid, Astronomy and Astrophysics, numerical [methods], Planetary system, Asteroids, asteroids: general, general [asteroids], Meteorite, physical evolution [planets and satellites], Space and Planetary Science, Asteroid, minor planets, CIENCIAS NATURALES Y EXACTAS, Astrophysics - Earth and Planetary Astrophysics
Abstract

Most meteorites are fragments from recent collisions experienced in the asteroid belt. In such a hypervelocity collision, the smaller collision partner is destroyed, whereas a crater on the asteroid is formed or it is entirely disrupted, too. The present size distribution of the asteroid belt suggests that an asteroid with a 100 km radius is encountered 1014 times during the lifetime of the solar system by objects larger than 10 cm in radius; the formed craters cover the surface of the asteroid about 100 times. We present a Monte Carlo code that takes into account the statistical bombardment of individual infinitesimally small surface elements, the subsequent compaction of the underlying material, and the formation of a crater and a regolith layer. For the entire asteroid, 10,000 individual surface elements are calculated. We compare the ejected material from the calculated craters with the shock stage of meteorites with low petrologic type and find that these most likely stem from smaller parent bodies that do not possess a significant regolith layer. For larger objects, which accrete a regolith layer, a prediction of the thickness depending on the largest visible crater can be made. Additionally, we compare the crater distribution of an object initially 100 km in radius with the shape model of the asteroid (21) Lutetia, assuming it to be initially formed spherical with a radius that is equal to its longest present ellipsoid length. Here we find the shapes of both objects to show resemblance to each other., Facultad de Ciencias Astronómicas y Geofísicas, Instituto Argentino de Radioastronomía

Published
2016

48. A polarimetric study of asteroids: Fitting phase-polarization curves

Author

Alberto Cellino, Edward F. Tedesco, M. Canada-Assandri, Ricardo Gil-Hutton, Paolo Tanga, Stefano Bagnulo, ITA, USA, GBR, FRA, and ARG

Subjects
Physics, POLARIZATION, 010504 meteorology & atmospheric sciences, Ciencias Físicas, Polarimetry, Astronomy and Astrophysics, Astrophysics, purl.org/becyt/ford/1.3 [https], Polarization (waves), GENERAL [ASTEROIDS], 01 natural sciences, Astronomía, purl.org/becyt/ford/1 [https], MINOR PLANETS, Space and Planetary Science, Asteroid, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, CIENCIAS NATURALES Y EXACTAS, 0105 earth and related environmental sciences
Abstract

By considering all published asteroid linear polarization data available in the literature, it is possible to obtain updated phase-polarization curves for several tens of objects. In a separate paper, we have produced new calibrations of different relations between the geometric albedo and several polarimetric parameters, based on an analysis of a limited sample of asteroids for which the albedo is known with sufficient accuracy. In this paper, we present the main polarization parameters and corresponding albedos for a larger data set of asteroids which we did not use for calibration purposes. We find a good agreement between the albedo values computed using different polarization parameters. Conversely, in the case of the so-called Barbarian asteroids the situation is rather unclear. Moreover, we present an updated analysis of the distributions of different polarimetric parameters, including the so-called inversion angle and the solar phase angle corresponding to the extreme value of negative polarization, and study their mutual relations. We find that the above parameters can be used to clearly distinguish some unusual classes of asteroids. Polarimetric parameters are known to be related to physical properties of asteroid surfaces which are difficult to infer by means of other observing techniques. By using a much larger data set, in our analysis we confirm and extend some results obtained in the past by other authors, and we explore more systematically some features that had been mostly unexplored before, mainly concerning the morphology of the negative polarization branch. Fil: Cellino, A.. Istituto Nazionale Di Astrofisica; Italia. Osservatorio Astrofisico di Torino; Italia Fil: Bagnulo, S.. College Hill; Reino Unido Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina Fil: Tanga, P.. Observatoire de la Cote D'Azur; Francia Fil: Cañada Assandri, Marcela Inés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina Fil: Tedesco, E. Planetary Science Institute; Estados Unidos

Published
2016

49. The Euphrosyne family's contribution to the low albedo near-Earth asteroids

Author

James Bauer, C. R. Nugent, Valerio Carruba, Joseph R. Masiero, A. K. Mainzer, CALTECH, and Universidade Estadual Paulista (Unesp)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Near-Earth object, Population, Comet, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Albedo, Asteroid family, general [asteroids], Secular resonance, Jupiter, Space and Planetary Science, Asteroid, minor planets, education, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Euphrosyne asteroid family is uniquely situated at high inclination in the outer Main Belt, bisected by the nu_6 secular resonance. This large, low albedo family may thus be an important contributor to specific subpopulations of the near-Earth objects. We present simulations of the orbital evolution of Euphrosyne family members from the time of breakup to the present day, focusing on those members that move into near-Earth orbits. We find that family members typically evolve into a specific region of orbital element-space, with semimajor axes near ~3 AU, high inclinations, very large eccentricities, and Tisserand parameters similar to Jupiter family comets. Filtering all known NEOs with our derived orbital element limits, we find that the population of candidate objects is significantly lower in albedo than the overall NEO population, although many of our candidates are also darker than the Euphrosyne family, and may have properties more similar to comet nuclei. Followup characterization of these candidates will enable us to compare them to known family properties, and confirm which ones originated with the breakup of (31) Euphrosyne., Accepted for publication in ApJ

Published
2015

50. Sublimation-Driven Activity in Main-Belt Comet 313P/Gibbs

Author

Richard J. Wainscoat, Bryce Bolin, Henry H. Hsieh, Lawrence H. Wasserman, Nader Haghighipour, Bojan Novaković, Pedro Lacerda, Jan Kleyna, Adam Waszczak, Eva Schunova, Olivier Hainaut, Alan Fitzsimmons, Marco Micheli, Nick Moskovitz, Colin Snodgrass, Larry Denneau, Karen J. Meech, and Rosita Kokotanekova

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Brightness, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Asteroid family, Precovery, individual: 313P&Gibbs [comets], general [comets], general [asteroids], Lyapunov time, Space and Planetary Science, Sky, minor planets, Sublimation (phase transition), Great conjunction, Subaru Telescope, media_common, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present an observational and dynamical study of newly discovered main-belt comet 313P/Gibbs. We find that the object is clearly active both in observations obtained in 2014 and in precovery observations obtained in 2003 by the Sloan Digital Sky Survey, strongly suggesting that its activity is sublimation-driven. This conclusion is supported by a photometric analysis showing an increase in the total brightness of the comet over the 2014 observing period, and dust modeling results showing that the dust emission persists over at least three months during both active periods, where we find start dates for emission no later than 2003 July 24+/-10 for the 2003 active period and 2014 July 28+/-10 for the 2014 active period. From serendipitous observations by the Subaru Telescope in 2004 when the object was apparently inactive, we estimate that the nucleus has an absolute R-band magnitude of H_R=17.1+/-0.3, corresponding to an effective nucleus radius of r_e~1.00+/-0.15 km. The object's faintness at that time means we cannot rule out the presence of activity, and so this computed radius should be considered an upper limit. We find that 313P's orbit is intrinsically chaotic, having a Lyapunov time of T_l=12000 yr and being located near two 3-body mean-motion resonances with Jupiter and Saturn, 11J-1S-5A and 10J+12S-7A, yet appears stable over >50 Myr in an apparent example of stable chaos. We furthermore find that 313P is the second main-belt comet, after P/2012 T1 (PANSTARRS), to belong to the ~155 Myr old Lixiaohua asteroid family., 8 pages, 4 figures; accepted for publication in ApJ Letters

Published
2015

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